Space Travel Under Constant 1g Acceleration

The basic principle behind every high-thrust interplanetary space probe is to accelerate briefly and then coast, following an elliptical, parabolic, or mildly hyperbolic solar trajectory to your destination, using gravity assists whenever possible. But this is very slow.

Imagine, for a moment, that we have a spacecraft that is capable of a constant 1g (“one gee” = 9.8 m/s2) acceleration. Your spacecraft accelerates for the first half of the journey, and then decelerates for the second half of the journey to allow an extended visit at your destination. A constant 1g acceleration would afford human occupants the comfort of an earthlike gravitational environment where you would not be weightless except during very brief periods during the mission. Granted such a rocket ship would require a tremendous source of power, far beyond what today’s chemical rockets can deliver, but the day will come—perhaps even in our lifetimes—when probes and people will routinely travel the solar system in just a few days. Journeys to the stars, however, will be much more difficult.

The key to tomorrow’s space propulsion systems will be fusion and, later, matter-antimatter annihilation. The fusion of hydrogen into helium provides energy E = 0.008 mc2. This may not seem like much energy, but when today’s technological hurdles are overcome, fusion reactors will produce far more energy in a manner far safer than today’s fission reactors. Matter-antimatter annihilation, on the other hand, completely converts mass into energy in the amount given by Einstein’s famous equation E = mc2. You cannot get any more energy than this out of any conceivable on-board power or propulsion system. Of course, no system is perfect, so there will be some losses that will reduce the efficiency of even the best fusion or matter-antimatter propulsion system by a few percent.

How long would it take to travel from Earth to the Moon or any of the planets in our solar system under constant 1g acceleration for the first half of the journey and constant 1g deceleration during the second half of the journey? Using the equations below, you can calculate this easily.

Keep in mind that under a constant 1g acceleration, your velocity quickly becomes so great that you can assume a straight-line trajectory from point a to point b anywhere in our solar system.

Maximum velocity is reached at the halfway point (when you stop accelerating and begin decelerating) and is given by

The energy per unit mass needed for the trip (one way) is then given by

How much fuel will you need for the journey?

hydrogen fusion into helium gives: Efusion = 0.008 mfuel c2

matter-antimatter annihilation gives: Eanti = mfuel c2

This assumes 100% of the fuel goes into propelling the spacecraft, but of course there will be energy losses and operational energy requirements which will require a greater amount of fuel than this. Moreover, we are here calculating the amount of fuel you’ll need for each kg of payload. We would need to use calculus to determine how much additional energy will be needed to accelerate the ever changing amount of fuel as well. The journey may well be analogous to the traveler not being able to carry enough water to survive crossing the desert on foot.

Now, let’s use the equations above for a journey to the nearest stars. There are currently 58 known stars within 15 light years. The nearest is the triple star system Alpha Centauri A & B and Proxima Centauri (4.3 ly), and the farthest is LHS 292 (14.9 ly).

I predict that interstellar travel will remain impractical until we figure out a way to harness the vacuum energy of spacetime itself. If we could extract energy from the medium through which we travel, we wouldn’t need to carry fuel onboard the spacecraft.

We already do something analogous to this when we perform a gravity assist maneuver. As the illustration below shows, the spacecraft “borrows” energy by infinitesimally slowing down the much more massive Jupiter in its orbit around the Sun and transferring that energy to the tiny spacecraft so that it speeds up and changes direction. When the spacecraft leaves the gravitational sphere of influence of Jupiter, it is traveling just as fast as it did when it entered it, but now the spacecraft is farther from the Sun and moving faster than it would have otherwise.

Reference: https://www.daviddarling.info/encyclopedia/G/gravityassist.html

Of course, our spacecraft will be “in the middle of nowhere” traveling through interstellar space, but what if space itself has energy we can borrow?

Satellite, Meteor, and Aircraft Crossings 2019

Edmund Weiss (1837-1917) and many astronomers since have called asteroids “vermin of the sky”, but on October 4, 1957 another “species” of sky vermin made its debut: artificial satellites.  In the process of video recording stars for possible asteroid occultations, I frequently see satellites passing through my ~¼° field of view.

I’ve put together a video montage of satellites I serendipitously recorded between March 31, 2019 and July 12, 2019.  Many of the satellite crossings are moving across the fields as “dashes” because of the longer integration times I need to use for some of my asteroid occultation work. A table of these events is shown below the video. The range is the distance between observer and satellite at the time of observation.

Satellites in higher orbits take longer to cross the field. When possible, I’ve included graphs of brightness as a function of time for these slower-moving satellites after each individual video and corresponding table. When you watch the videos of geostationary satellites, you are actually seeing the rotation of the Earth as the line between you and the satellite sweeps across the stars as the Earth rotates!

Uncertain of identification
A tumbler with sun glints!
A high-amplitude tumbler! Satellite is no longer operational.

I caught one meteor on 4 Jan 2019 between 5:32:57 and 5:32:59 UT. Field location was UCAC4 419-017279. I’m pretty sure the meteor was a Quadrantid!

And two aircraft crossed my field: on 7 Dec 2018 1:40:05 – 1:40:13 UT (UCAC4 563-026131) and 26 Jun 2019 5:02:07 – 5:02:10 UT (UCAC4 291-144196).

And high energy particles (natural radioactivity or cosmic rays) “zing” my CCD/CMOS detector every once in a while. Here are a few examples: 5 Jan 2019 3:46:00 – 3:46:02 UT (UCAC4 473-001074); 20 Apr 2019 3:41:46 – 3:41:47 UT (UCAC4 501-062663); 30 Jun 2019 7:37:31 – 7:37:33 (UCAC4 354-179484) and 7:47:41 – 7:46:44 (TYC 6243-00130-1).

References
Hughes, D. W. & Marsden, B. G. 2007, J. Astron. Hist. Heritage, 10, 21

Asteroids: Take a Number

Italian monk, mathematician, and astronomer Giuseppe Piazzi (1746-1826) discovered an unexpected 8th magnitude object in Taurus near Mars and the Pleiades at around 8:00 p.m. on January 1, 1801 at his observatory in Palermo, Sicily. Thinking it a comet, he recorded the position of the object over several nights, until illness forced him to quit on February 11, just a few days after the object passed fairly close to Mars. By early May, the object was too close to the Sun in the western sky to observe, and Piazzi despaired of ever recovering the object. The now-famous 24-year-old German mathematician Carl Gauss (1777-1855) came to the rescue. Gauss used Piazzi’s positions to determine an orbit for Ceres (so named by Piazzi) and predicted from the scant data its future positions when it would once again be visible in the night sky. Ceres was recovered only a half-degree away from its predicted position by Hungarian astronomer Franz Xaver von Zach (1754-1832) on December 7, close to Denebola and not far from a close conjunction of the planets Jupiter and Saturn, and then confirmed after a long stretch of cloudy weather on December 31, 1801. The German amateur astronomer Heinrich Olbers (1758-1840) found Ceres at Bremen two days later on January 2, 1802. Olbers (of Olbers’ Paradox fame) discovered the second asteroid, Pallas, on March 28, 1802. Many, many more asteroids have been discovered since then. They are sequentially numbered, originally in order of their discovery date, but nowadays in order of their receiving a precise orbit determination.

Fast forward.

The names of asteroids 998 through 1002, discovered between August 6-15, 1923, have special significance.

998 Bodea – named in honor of German astronomer Johann Elert Bode (1747-1826), whose empirical relationship of the distances of the planets (Titius-Bode Law) indicated that there should be a planet between the orbits of Mars and Jupiter, touching off a massive search led by von Zach for a new planet.

999 Zachia – named in honor of Franz Xaver von Zach, who published Piazzi’s observations and recovered Ceres after Gauss’ predicted positions.

1000 Piazzia – named in honor of Giuseppe Piazzi, who discovered the first asteroid, 1 Ceres.

1001 Gaussia – named in honor of Carl Friedrich Gauss, who predicted the position of Ceres so it could be recovered.

1002 Olbersia – named in honor of Heinrich Olbers who was the second person to recover Ceres and the discoverer of the second asteroid, 2 Pallas (and 4 Vesta, by the way).

Fortunately, German astronomer Johann Daniel Titius (1729-1796) finally did get an asteroid named after him as well: 1998 Titius, discovered on February 24, 1938.

As of August 19, 2019, 796,422 minor planets (asteroids, trans-Neptunian objects, etc., but not including comets) have been discovered, but only 541,128 have orbits that are well-enough determined that they have been given a minor planet number. When a minor planet is first discovered, it is given a provisional designation based on the date of discovery. For example, 2019 PE3 was discovered during the first half of August 2019. After enough high-quality astrometric data has been collected to determine an accurate orbit, the minor planet is assigned a number. For example, minor planet 1996 TB1 was discovered by IOTA member George Viscome on October 5, 1996. It received a number, 35283, in 2000, and it received a name, Bradtimerson, earlier this year (2019). George submitted the name to the IAU after Brad Timerson, mentor and inspiration to many of the current crop of asteroid occultation observers, passed away on October 17, 2018. So we now have 35283 Bradtimerson.

The counts in the paragraph above show us that 67.9% of the minor planets that have been discovered have been assigned a number. Of these, only 21,922 (4.1%) have received a name.

Many asteroids have been given interesting or unusual names. Excluding the many fine individuals (real, not fictional) who have an asteroid named after them, here are a few of my favorites. There are a few here that are actually named after a person, but the minor planet name has a meaning beyond just the person’s name.

Remember, these are real places that will be visited someday. Oh, to be so lucky!

Lots of asteroids are awaiting names. Can you come up with some interesting, entertaining, or poetic ones? Give it a try, check this list or do a search here to make sure it is new, and then post a comment here and I’ll probably include your ideas in this article, giving you credit, of course. Be creative!

To get you in the spirit, here are a few names I’ve come up with:

  • Botanica
  • Distantia
  • Eternium
  • Gandalf
  • Luminaria
  • Morethanamote
  • Portentia
  • Symphonica

Have fun!

Cometary Tails

A comet’s ion/plasma/gas tail points directly away from the Sun. A comet’s dust tail deviates somewhat (and sometimes a lot) from this, falling behind the comet along its orbital path around the Sun.

For the best view of either tail, our line of sight should be perpendicular to the length of the tail. However, that seldom happens, and we are viewing the tails with some degree of foreshortening. The orientation of the gas tail is called the phase angle, and it is the Sun – comet – observer angle.

A phase angle of 0° indicates we are looking straight down the tail of the comet (maximum foreshortening) with the head being oriented closest to the observer.

A phase angle of 90° indicates that our line-of-sight to the comet is perpendicular to the Sun-comet line, so we are viewing the comet’s gas tail with no foreshortening.

A phase angle of 180° indicates that we are again looking straight down the gas tail of the comet (again, maximum foreshortening) only this time the tail is closer to the observer and the head further away. Of course, the only time this orientation could happen is when the comet is transiting the Sun, thus rendering it essentially unobservable.

Phase angles of 0 to 90° mean that the comet head is closer to the observer than the tail; angles of 90 – 180° mean that the comet’s tail is closer to the observer than the head.

Here’s a table showing the phase angle, and some other information, for currently-observable comets brighter than 15th magnitude as seen from Earth. The column labeled Elongation indicates the Sun – observer – comet angle. In other words, the angular separation between the Sun and the comet.

A comet that is farther from the Sun than the observer can never have a phase angle as great as 90°, but a comet that is closer to the Sun than the observer can. Looking at the diagram above and considering a comet in a circular orbit around the Sun (highly unlikely, I know, but bear with me) and closer to the Sun than the observer, the phase angle would be 90° when the comet is at greatest elongation.

Incidentally, comet designations that have a number followed by the letter “P” (such as 29P, 68P, and 260P) are periodic comets (more precisely described as short-period comets), defined to be comets with orbital periods of less than 200 years or that have been observed at more than one perihelion passage.

Anyone Need a Good SAS Programmer?

My current company, despite my objections and expertise, is phasing out SAS, and I think it is a misguided decision.

I am only about three years away from semi-retirement, but you won’t find a more motivated worker.  Not only am I a top flight SAS programmer with many years of experience, but I’m also very good at teaching and mentoring others in the use of SAS—something I almost never get to do in my current position.

I need a change.

I have “big city” job skills in a small town where there appear to be no other employers who would be able to make use of my SAS expertise.  And, at this stage of my life, I can’t relocate and am unwilling to commute, so working from home appears to be the only option.

I’m looking at potential opportunities as an “encore career” and would really like to do something that directly benefits society.  I loved my 21 years at the Iowa Department of Transportation, and would love to be a public servant once again, or to work for a nonprofit organization. Or work on scientific projects—true science, not data “science”. Or, data for good projects.  Both salary and number of work hours (up to full time) are completely negotiable.  I’m at a point now in my career where I can be more flexible for the right opportunity.

I have my own personal SAS Analytics Pro license, so could do work for you even if you don’t have SAS.

SAS is a great product, and SAS Institute is a great company.  And SAS keeps getting better all the time.

Some say that SAS is difficult to learn, but, like many things, it is not difficult at all if you have a good teacher who has a thorough understanding of the subject matter and a passion for teaching it. That would be me.

Scythia Sweet

One of the enjoyable aspects of recording asteroids passing in front of stars (we call them asteroid occultations) is the interesting names of some of the asteroids. This month, Bob Dunford, Steve Messner, and I had two double-chord events across the asteroid 1306 Scythia, discovered in this month of 1930 by Soviet astronomer Grigory Neujmin (1886-1946).

The name 1306 Scythia immediately brought to mind a favorite piece of music, the Scythian Suite—surely one of the most unusual and otherworldly compositions by Sergei Prokofiev, or anyone else for that matter.

A quick look at the entry for 1306 Scythia in the 5th edition of Dictionary of Minor Planet Names by Lutz D. Schmadel (1942-2016) quickly confirmed my suspicion that the subject matter of both asteroid and musical composition is the same.

Named for the country of the ancient Scythians comprising parts of Europe and Asia now in the U.S.S.R. in regions north of the Black sea and east of the Aral sea.

In the wee hours of Friday, July 12, Bob Dunford in Illinois and I in Wisconsin observed only the second asteroid occultation of 1306 Scythia (and the first since 2014). The predicted path is shown below.

Predicted shadow path of the asteroid 1306 Scythia from the star Tycho 5189-597-1 (UCAC4 414-136241) on 12 July 2019 UT.

Bob, who was observing at Naperville, observed a 4.3-second dip in brightness as the asteroid covered the star between 8:23:46.203 and 8:23:50.531 UT, and I, observing at Dodgeville, observed a 1.3-second event between 8:24:01.783 and 8:24:03.054. Our light curves are shown below.

Bob Dunford’s light curve of the 1306 Scythia / Tycho 5189-597-1 event of 12 July 2019 UT, using a 14-inch telescope.
David Oesper’s light curve of the 1306 Scythia / Tycho 5189-597-1 event of 12 July 2019 UT, using a 12-inch telescope.

Here’s a map showing our observing locations relative to the predicted path.

1306 Scythia / Tycho 5189-597-1 event of 12 July 2019 UT – Predicted Path and Observer Locations

Here’s the profile showing the chords across the asteroid.

1306 Scythia / Tycho 5189-597-1 event of 12 July 2019 UT – Asteroid Profile and Chords

Just four days later, both Bob Dunford and I had a high probability event of the same asteroid passing in front of a different star, and this time we were joined by Steve Messner. Bob and Steve both got positives! Unfortunately, I was clouded out.

Predicted shadow path of the asteroid 1306 Scythia from the star TYC 5188-573-1 on 16 July 2019 UT.
1306 Scythia / Tycho 5188-573-1 event of 16 July 2019 UT – Predicted Path and Observer Locations
1306 Scythia / Tycho 5188-573-1 event of 16 July 2019 UT – Asteroid Profile and Chords

Sergei Prokofiev (1891-1953) wrote the Scythian Suite in 1915 when he was 24 years of age. Even at that young age, Prokofiev already showed great talent and originality.

Sergei Prokofiev, circa 1918

Here are some excerpts of the Scythian Suite performed by the Minnesota Orchestra conducted by Stanisław Skrowaczewski. This is a 1983 recording (Vox Box CD3X 3016). The movement descriptions are based on those given in Wikipedia.

1st movement: Invocation to Veles and Ala – barbaric and colorful music describing the Scythians’ invocation of the sun.

Some of the music you’ve heard in the original “Star Trek” certainly was inspired by this.
Alien landscape music
Alien landscape music #2

2nd movement: The Alien God and the Dance of the Evil Spirits – as the Scythians make a sacrifice to Ala, daughter of Veles, the Alien God performs a violent dance surrounded by seven monsters.

Best to observe this nasty dance from a distance…
This certainly reminds me of Dmitri Shostakovich, but he was only 9 years old at the time and just beginning to compose!

3rd movement: Night – the Alien God harms Ala; the Moon Maidens descend to console her.

This beautiful movement of many moods begins peacefully, then moves to a section of descending lines that might remind you of “The Planets” by Gustav Holst, but this was being written at the exact same time as the Scythian Suite! Next the music takes an ominous turn, and then returns to a little night music, but more a travel through interstellar or intergalactic space rather than a terrestrial night.

4th movement: The Glorious Departure of Lolli and the Cortège of the Sun – Lolli, the hero, comes to save Ala; the Sun God assists him in defeating the Alien God. They are victorious, and the suite ends with a musical picture of the sunrise.

Here, now, the conclusion of this remarkable work.

Prokofiev’s Scythian Suite. There is nothing else like it in the orchestral repertoire!

Dodgeville Streetlights

Has anyone else noticed how Alliant Energy is gradually replacing our orangish-white-light streetlights with bluish-white-light ones? The orangish-white-light streetlights are high-pressure sodium (HPS) with a correlated color temperature (CCT) of 1900K, whereas the bluish-white-light streetlights that are replacing them are LED with a CCT of 4000K, and, most notably, they are two and a half times as bright.

Even though I have written to both Alliant Energy and the City of Dodgeville, nothing has changed.

My questions, which are still unanswered:

What is the justification for increasing the streetlighting illumination level by two and a half times over what it has been for decades?

Why are we going from 1900K to 4000K (cold white), when 2700K or 3000K (warm white) is readily available and being used in many communities in the U.S. and Canada?

This same transformation is happening in Mineral Point, and probably many other communities in SW Wisconsin as well.

Is anyone else noticing how this is profoundly changing the rural character of our nighttime environment? Is anyone else concerned about this? The increase in glare and light trespass onto neighboring properties from these new LED lights is quite noticeable to me, even though they are nominally full-cutoff. Why? They are too bright, and too blue.

If anyone locally is reading Cosmic Reflections (and sometimes I wonder if anyone is…), and if you have noticed and are alarmed by these streetlighting changes, please contact me on blog or off blog (oesper at mac.com) and let’s meet and discuss a plan of action. Something needs to be done before it is too late and we are stuck with this very negative change to our nighttime environment.

Dark-Sky Communities

Back in 2006, I started a Yahoo! Group called DarkSkyCommunities. My goal was to provide a forum for astronomy enthusiasts and other like-minded individuals to discuss living where you’d have a star-filled night sky and never have to worry about streetlights or neighbor’s lights. Everyone else in the community would value the night sky and a natural nighttime environment as you do.

My approach with DarkSkyCommunities was not to be a heavy-handed moderator. I approved new members but after that, members were free to post (within reason) anything they wanted to. In that sense, it worked pretty well and there were very few postings I ever had to take down.

Unfortunately, astronomers know next to nothing about intentional community and intentional communitarians know next to nothing about astronomy, so the group drifted far from my original intent to a general discussion about light pollution, with “what’s wrong with the IDA” being a surprisingly popular topic for discussion. Eventually, though, a small number of individuals with a chip on their shoulder or an axe to grind became the most frequent posters, and that sort of poisoned the group.

So, I’d like to introduce to you DarkSkyCommunities 2.0: a Google group called Dark-Sky Communities. Here’s the description on the landing page:

Dark-Sky Communities is a discussion group for the development and nurturing of intentional communities where the night sky and the nighttime environment are valued and protected. The emphasis is on affordable, sustainable dark-sky communities where those of modest financial means can live, work, and retire. This group is moderated to keep the focus on intentional communities that are astronomy-friendly.

This time around I am going to approve (or disapprove) the messages posted to the group so that we stay on the topic of astronomy-friendly intentional communities. If you have an interest in this topic, please join!

Light pollution, despite our best efforts, is getting worse almost everywhere. LED lighting which had (and still has) so much promise is generally resulting in more lights, brighter lights, and bluer lights—not the direction we want to head.

Someday, I would like to live in a place where I can walk a few feet beyond my door, set down a lawn chair, and watch a meteor shower without being assaulted by streetlights, insecurity lights, glare, and skyglow. Is that too much to ask?

Would you like to live in a place like that, too? Let’s make it happen!

In Praise of Indexes

SAS Press recently discontinued selling physical books, and now offers publications only in an electronic format (EPUB, Kindle, and PDF). I’m sure this is not an isolated incident and many other smaller publishing houses are going the same route.

I recently purchased the 3rd edition of Kirk Paul Lafler’s useful book, PROC SQL: Beyond the Basics Using SAS. I have the first and second editions of his book in softcover, and I was pleased to find that I could order a physical copy of his third edition through Amazon. After receiving the book, I quickly discovered that the third edition no longer includes an index!

I contacted SAS about the omission of the index, and received a prompt and courteous reply:

“You are correct about the index.  Indexes are no longer a standard part of our print books.  I do understand your concern, and have forwarded your feedback to the appropriate editors. All of our e-books are searchable. If you would like a complimentary copy of the corresponding e-book, I will be happy to forward that to you.”

I learned that neither the hardcopy nor the electronic version of the book contains an index.

I know I am 63 years old, and maybe not as immersed in modern technology as my younger colleagues, but since when did an index become a dispensable part of any non-fiction book?

First page of the index of PROC SQL: Beyond the Basics Using SAS, Second Edition

A good index is like a table of contents, only much more detailed. Sure, you can search a PDF for a particular term, but what if you can’t think of the term you’re searching for? For example, you might not remember that the type of many-to-many join you are looking for is called a Cartesian product, but when you see this term in the index it jogs your memory and you can find it on pages 237 and 242, which then leads you to the term cross join.

Another problem with searching through a document is that I have yet to see any search provide the ability to search for more than one non-contiguous terms at a time on a page or adjacent pages. A well-crafted index is often more effective than one-dimensional searching at finding topics that can’t easily be reduced to a single word or term.

Index subheadings, such as shown for CASE expressions above, are also hard to replace with one-dimensional searching.

Indexing is so important and requires such skill (to do it right) that there is even a professional organization for it: the American Society for Indexing.

I hope you can see now that every non-fiction book, printed or electronic, needs an index to help you quickly find the information you need.

Notes from AAS 234

I attended the 234th meeting of the American Astronomical Society (AAS), held in St. Louis, Missouri, June 9-13, 2019. Here are some highlights from that meeting.

Day 1 – Monday, June 10, 2019

Research Notes of the AAS is a non-peer-reviewed, indexed and secure record of works in progress, comments and clarifications, null results, or timely reports of observations in astronomy and astrophysics. RNAAS.

The Bulletin of the American Astronomical Society is the publication for science meeting abstracts, obituaries, commentary articles about the discipline, and white papers of broad interest to our community. BAAS.

We still have many unanswered questions about galaxy formation. The rate of star formation in galaxies and central black hole accretion activity was highest between 10 and 11 billion years ago. This corresponds to redshift z around 2 to 3, referred to as “cosmic high noon”. This is the ideal epoch for us to answer our questions about galaxy formation. Near-infrared spectroscopy is important to the study of galaxies during this epoch, and we are quite limited in what we can do from terrestrial observatories. Space based telescopes are needed, and the James Webb Space Telescope (JWST) will be key.

Galaxies are not closed boxes. We need to understand how inflows and outflows affect their evolution (“galactic metabolism”).

There are five international space treaties, with the Outer Space Treaty of 1967 being the first and most important. The United States has signed four of the five treaties. The Moon Agreement of 1979 which states that no entity can own any part of the Moon does not include the United States as one of the signatories.

U.S. Code 51303, adopted in 2015, identifies asteroid resource and space resource rights, and states that “A United States citizen engaged in commercial recovery of an asteroid resource or a space resource under this chapter shall be entitled to any asteroid resource or space resource obtained, including to possess, own, transport, use, and sell the asteroid resource or space resource obtained in accordance with applicable law, including the international obligations of the United States.”

So, unfortunately, U.S. law does allow a commercial entity to own an asteroid, but you have to get there first before you can claim it. The large metallic asteroid 16 Psyche is highly valuable and will probably be owned by some corporation in the not-too-distant future.

Space law often relies upon maritime law as a model.

Astronomer Vayu Gokhale from Truman State University gave an interesting iPoster Plus presentation on how he and his students are operating three automated and continuous zenithal sky brightness measurement stations using narrow-field Sky Quality Meters (SQMs) from Unihedron. Even measurements when it is cloudy are of value, as clouds reflect light pollution back towards the ground. Adding cloud type and height would allow us to make better use of cloudy-night sky brightness measurements. In a light-polluted area, the darkest place is the zenith, and clouds make the sky brighter. In an un-light-polluted area, the darkest place is the horizon, and clouds make the sky darker.

A number of precision radial velocity instruments for exoplanet discovery and characterization will begin operations soon or are already in operation: NEID, HARPS, ESPRESSO, EXPRES, and iLocater, to name a few.

Dark matter: clumps together under gravity, does not emit, reflect, or absorb electromagnetic radiation, and does not interact with normal matter in any way that causes the normal matter to emit, reflect, or absorb electromagnetic radiation. The ratio between dark matter and normal (baryonic matter) in our universe is 5.36 ± 0.05 (Planck 2018).

What is dark matter? It could be a new particle. If so, can we detect its non-gravitational interactions? It could be macroscopic objects, perhaps primordial black holes. Or, it could be a mixture of both. Another possibility is that a modification to the laws of gravitation will be needed to mimic the effects of dark matter.

How “dark” is dark matter? Does it interact at all (besides gravitationally)? Can dark matter annihilate or decay? Even if dark matter started hot, it cools down rapidly as the universe expands.

Primordial black holes could have masses ranging anywhere between 10-16 and 1010 solar masses. LIGO is possibility sensitive to colliding primordial black holes with masses in the range of a few to a few hundred solar masses. Primordial black holes are a fascinating dark matter candidate, with broad phenomenology.

The Cosmic Microwave Background (CMB) is a nearly perfect blackbody with distortions < 1 part in 10,000. What this tells us is that nothing dramatically heated or cooled photons after 2 months after the Big Bang. Anisotropies are variances in the CMB temperature, and the angular power spectrum is variance of CMB temperature as a function of angular scale. CMB anisotropies are very sensitive to the ionization history of the universe. How the universe recombined plays a key role in CMB anisotropies.

Hydrogen: not such a simple atom.

The CMB is polarized. The polarization is caused by Mie scattering of photons.

At the NASA Town Hall, we learned about current and future missions: TESS, SPHEREx, HabEx, LUVOIR, Lynx, Origins Space Telescope (OST).

The highest image rate of standard CCD and CMOS video cameras for asteroid occultation work is 30 frames (60 fields) per second, providing time resolution of 0.017 seconds per field. Adaptive optics and autoguider imaging devices often have a higher sampling rate, and such a camera could perhaps be easily modified to be used for occultation work. A time-inserter would need to be added to the camera (either on-board or GPS-based), and improvements in quantum efficiency (because of the shorter exposures) would benefit from newer imaging technologies such as a Geiger-mode avalanche photodiode (APD); or the Single-photon avalanche detector (SPAD), which are frequently used in chemistry.

Gregory Simonian, graduate student at Ohio State, presented “Double Trouble: Biases Caused by Binaries in Large Stellar Rotation datasets”. The Kepler data yielded 34,030 rotation periods through starspot variability. However, the rapid rotators are mostly binaries. In the Kepler dataset, many rapid rotators have a spin period of the stars equal to the orbital period of the binary. These eclipsing binaries, also known as photometric binaries because they are detected through changes in brightness during eclipses and transits, need to be treated separately in stellar rotation datasets.

Granulation was discovered by William Herschel in 1801 and are vertical flows in the solar photosphere on the order of 1000 m/s, and 1000 km horizontal scale. Supergranulation (Hart 1954, Leighton et al. 1962) are horizontal motions in the photosphere of 300 to 500 m/s with a horizontal scale on the order of 30,000 km.

The amplitude of oscillations in red giants increase dramatically with age.

We’ve never observed the helium flash event in a red giant star, though models predict that it must occur. It is very brief and would be difficult to detect observationally.

Brad Schaefer, Professor Emeritus at Louisiana State University, gave a talk on “Predictions for Upcoming Recurrent Nova Eruptions”. Typically, recurrent novae have about a 30% variation in eruptive timescales, so predicting the next eruption is not trivial. Due to the solar gap (when the object is too close to the Sun to observe on or near the Earth), we are obviously missing some eruptions. However, orbital period changes (O-C curve) can tell us about an eruption we missed. U Sco and T CrB are well-known examples of recurrent novae. Better monitoring of recurrent novae is needed during the pre-eruption plateau. Monitoring in the blue band is important for prediction.

I had the good fortune to talk with Brad on several occasions during the conference, and found him to be enthusiastic, knowledgeable, and engaging. Perhaps you have seen The Remarkable Science of Ancient Astronomy (The Great Courses), and he is just as articulate and energetic in real life. Among other things, we discussed how the internet is filled with misinformation, and even after an idea has been convincingly debunked, the misinformation continues to survive and multiply in cyberspace. This is a huge problem in the field of archaeoastronomy and, indeed, all fields of study. People tend to believe what they want to believe, never mind the facts.

Astrobites is a daily astrophysical-literature blog written by graduate students in astronomy around the world. The goal of Astrobites is to present one interesting paper from astro-ph per day in a brief format accessible to its target audience: undergraduate students in the physical sciences who are interested in active research.

Helioseismology can be done both from space (all) and the ground (some). Active regions on the far side of the Sun can be detected with helioseismology.

All HMI (Helioseismic and Magnetic Imager) data from the Solar Dynamics Observatory is available online.

A good approach to studying solar data is to subtract the average differential rotation at each point/region on the Sun and look at the residuals.

The Wilcox Solar Observatory has been making sun-as-a-star mean magnetic field measurements since 1975.

It is possible to infer electric currents on the Sun, but this is much more difficult than measuring magnetic fields.

Future directions in solar studies: moving from zonal averages to localized regions in our modeling, and the ability through future space missions to continuously monitor the entire surface of the Sun at every moment.

Systematic errors are nearly always larger than statistical uncertainty.

Day 2 – Tuesday, June 11, 2019

It is probably not hyperbole to state that every star in our galaxy has planets. About 1/5 of G-type stars have terrestrial planets within the habitable zone. Life is widespread throughout the universe.

Gas-grain interaction is at the core of interstellar chemistry. Interstellar ices, charged ices, surface chemistry – there is more time for interactions to occur on a dust grain than in a gas. Grain collisions are important, too.

Hot cores are transient regions surrounding massive protostars very early in their evolution. Similar regions are identified around low-mass protostars and are called corinos.

Methanol (CH3OH) is key to making simple organic molecules (SOM). Evaporating ice molecules drive rich chemistry. Dust plays a key role in the chemistry and in transporting material from the interstellar medium (ISM) to planetary systems.

The Rosetta mission detected amino acids on comet 67P/Churyumov–Gerasimenko.

JUICE (JUpiter ICy moons Explorer) is an ESA mission scheduled to launch in 2022, will enter orbit around Jupiter in October 2029 and Ganymede in 2032. It will study Europa, Ganymede, and Callisto in great detail.

The gravitational wave event GW170817 (two infalling and colliding neutron stars) was also detected as a gamma-ray burst (GRB) by the Fermi gamma-ray space telescope, which has a gamma-ray burst detector that at all times monitors the 60% of the sky that is not blocked by the Earth.

The time interval between the GW and GRB can range between tens of milliseconds up to 10 seconds.

The Milky Way galaxy circumnuclear disk is best seen at infrared wavelengths around 50 microns. Linear polarization tells us the direction of rotation. The star cluster near the MW center energizes and illuminates gas structures. Gravity dominates in this region. The role of magnetic fields in this region has been a mystery.

Pitch angle – how tightly wound the spiral arms are in a spiral galaxy.

Are spiral arms transient or long lived? They are probably long lived. There may be different mechanisms of spiral arm formation in grand design spirals compared with other types of spiral galaxies.

In studying spiral galaxies, we often deproject to face-on orientation.

The co-rotation radius is the distance from the center of a spiral galaxy beyond which the stars orbit slower than the spiral arms. Inside this radius, the stars move faster than the spiral arms.

The Sun is located near the corotation circle of the Milky Way.

The origins of supermassive black holes (SMBH) at the centers of galaxies are unclear. Were they seeded from large gas clouds, or were they built up from smaller black holes?

The black holes at the centers of spiral galaxies tend to be more massive when the spiral arm winding is tight, and less massive when the spiral arm winding is loose.

Spiral Graph is in review as a Zooniverse project and has not yet launched. Citizen scientists will trace the spiral arms of 6,000 deprojected spiral galaxies, and 15 traces will be needed for each galaxy. Spiral arm tracings will provide astronomers with intermediate mass black hole candidate galaxies.

Barred spiral galaxies are very common. 66% to 75% of spiral galaxies show evidence of a bar at near-infrared wavelengths.

Magnetic fields in the inner regions of spiral galaxies are scrambling radio emissions to some extent, but radio astronomers have ways to deal with this.

For me, the plenary lecture given by Suvrath Mahadevan, Pennsylvania State University, was the first truly outstanding presentation. His topic was “The Tools of Precision Measurement in Exoplanet Discovery: Peeking Under the Hood of the Instruments”. His discussion of the advance in radial velocity instrumentation was revelatory to me, as his starting point was Roger F. Griffin’s radial velocity spectrometer we used at Iowa State University in the 1970s and 1980s, giving us a precision of about 1 km/s. My, we have come a long way since then!

St. Louis, MO – AAS 2019 – Suvrath Mahadevan during the Plenary Lecture at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Tuesday June 11, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

To discover our Earth from another star system in the ecliptic plane would require detecting an 8.9 cm/s velocity shift in the Sun’s motion over the course of a year.

Precision radial velocity measurement requires we look at the displacement of thousands of spectral lines using high resolution spectroscopy.

The two main techniques are 1) Simultaneous reference and 2) Self reference (iodine cell). Also, externally dispersed interferometry and heterodyne spectroscopy can be used.

Griffin 1967 ~ km/s → CORAVEL 1979 ~300 m/s → CORALIE/ELODIE 1990 ~ 5-10 m/s → HARPS 2000 ~ 1 m/s → ESPRESSO/VLT, EXPRES/DCT, NEID/KPNO, HPF/HET.

We cannot build instruments that are stable over time at 10 cm/s resolution or less.

You can track the relative change in velocity much better than absolute velocity because of the “noise” generated by stellar internal motions.

Measuring the radial velocity at red or infrared wavelengths is best for M dwarfs, and cooler stars.

High radial velocity precision will require long-term observations, and a better understanding of and mitigation for stellar activity. Many things need to be considered: telescope, atmosphere, barycentric correction (chromatic effects can lead to 1/2 m/s error), fibers, modal noise, instrument decoupled from the telescope, calibrators, optics, stability, pipeline, etc. Interdisciplinary expertise is required.

NEID will measure wavelengths of 380 – 930 nm, and have a spectral resolution of R ~ 90,000.

Pushing towards 10 cm/s requires sub-milli-Kelvin instrument stability high-quality vacuum chambers, octagonal fibers, scrambling, and excellent guiding of the stellar image on the fiber to better than 0.05 arcseconds.

Precision radial velocity instruments such as NEID and HPF weigh two tons, so at present they can only be used with ground-based telescopes.

Charge Transfer Efficiency (CTE): need CCDs with CTE > 0.999999. Other CCD issues that don’t flat field out accurately: CCD stitch boundaries, cross hatching in NIR detectors, crystalline defects, sub-pixel quantum efficiency differences. Even the act of reading out the detector introduces a noise source.

10 cm/s is within reach from a purely instrumental perspective, but almost everything has to be just right. But we need to understand stellar activity better: granulation, supergranulation, flares, oscillations, etc. We may not be able to isolate these components of stellar activity, but we will certainly learn a lot in the process.

1s time resolution is required to properly apply barycentric corrections.

NASA’s Universe of Learning : Connecting Learners to the Subject-Matter Experts of NASA Astrophysics: https://www.universe-of-learning.org/

The OpenStax Astronomy Text: https://openstax.org/details/astronomy

Andrew Fraknoi gave an update on the OpenStax Astronomy text.

  • about 70 people have been involved in its development and vetting
  • each chapter includes collaborative group activities
  • math examples are in separate boxes
  • it is estimated that 500+ institutions have adopted this online and free introductory astronomy textbook, and ~200,000 students have used it, including ~30,000 amateur astronomers
  • multiple choice question bank for registered instructors
  • short videos with each chapter
  • available to everyone
St. Louis, MO – AAS 2019 – Attendees during the Eclipse Planning Workshop at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Sunday June 9, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

Open Educational Resources (OER): https://www.oercommons.org/

International Lunar Observatory Association (ILOA); http://www.spaceagepub.com/ ; https://galaxyforum.org/

The surface of the Moon has a thinner atmosphere than low-Earth orbit.

Kenneth Gayley, University of Iowa, gave an interesting short talk, “The Real Explanation for Type Ia Supernovae and the Helium Flash”. Here’s the abstract: https://ui.adsabs.harvard.edu/abs/2019AAS…23422404G/abstract . I’m looking forward to reading the entire paper.

Gene Byrd, University of Alabama, gave an interesting short presentation, “Two Astronomy Demos”. The first was “Stars Like Grains of Sugar”, reminiscent of Archimedes’ The Sand Reckoner. And “Phases with the Sun, Moon, and Ball”. He uses a push pin in a golf ball (the golf ball even has craters!). Morning works best for this activity. The Sun lights the golf ball and the Moon and they have the same phase—nice! Touching as well as seeing the golf ball helps students understand the phases of the Moon. Here’s a link to his paper on these two activities.

Daniel Kennefick, University of Arkansas, gave a short presentation on the 1919 eclipse expedition that provided experimental evidence (besides the correct magnitude of the perihelion precession of Mercury) that validated Einstein’s General Relativity. Stephen Hawking in his famous book A Brief History of Time mis-remembered that the 1979 re-analysis of the Eddington’s 1919 eclipse data showed that he may “fudged” the results to prove General Relativity to be correct. He did not! See Daniel Kennefick’s new book on the subject, No Shadow of a Doubt: The 1919 Eclipse That Confirmed Einstein’s Theory of Relativity.

St. Louis, MO – AAS 2019 – Daniel J. Kennefick during the Press Conference: Spiral Galaxies Near and Far at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Tuesday June 11, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

Brad Schaefer, Louisiana State University, gave another engaging talk, presenting evidence that the Australian aborigines may have discovered the variability of the star Betelgeuse, much earlier than the oft-stated discovery by John Herschel in 1836. Betelgeuse varies in brightness between magnitude 0.0 and +1.3 quasi-periodically over a period of about 423 days. It has been shown that laypeople can detect differences in brightness as small as 0.3 magnitude with the unaided eye, and with good comparison stars (like Capella, Rigel, Procyon, Pollux, Adhara, and Bellatrix—not all of which are visible from Australia—for Betelgeuse). It is plausible that the variability of Betelgeuse may have been discovered by many peoples at many different times. The Australian aborigines passed an oral tradition through many generations that described the variability of Betelgeuse. https://ui.adsabs.harvard.edu/abs/2019AAS…23422407S/abstract.

As a longtime astronomical observer myself, I have actually never noticed the variability of Betelgeuse, but Brad has. After his presentation, I mentioned to Brad that it would be interesting to speculate what would lead early peoples to look for variability in stars in the first place, which seems to me to be a prerequisite for anyone discovering the variability of Betelgeuse. His response pointed out that all it would take is one observant individual in any society who would notice/record the variability and then point it out to others.

During the last plenary session of the day, it was announced that the Large Synoptic Survey Telescope (LSST), which is expected to see first light in 2020, is expected to be renamed the Vera Rubin Survey Telescope. Tremendous applause followed! https://aas.org/posts/news/2019/06/lsst-may-be-renamed-vera-rubin-survey-telescope .

If you haven’t looked at the NASA/IPAC Extragalactic Database (NED) lately, you will find new content and functionality. It has been expanded a great deal, and now includes many stellar objects, because we don’t always know what is really a star and what is not. There is now a single input field where you can enter names, coordinates with search radius, etc. NED is “Google for Galaxies”.

I noticed during the 10-minute iPoster Plus sessions that there is a countdown timer displayed unobtrusively in the upper right hand corner that helps the presenter know how much time they have remaining. I think this would be a great device for anyone giving a short presentation in any venue.

St. Louis, MO – AAS 2019 – Attendees during the iPosters/iPosters Plus at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Monday June 10, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

Galactic archaeology is the study of the oldest stars and other structures in our galaxy to better understand how our galaxy evolved.

The AAS has a YouTube channel: https://www.youtube.com/channel/UChXuQtcWbViLxCnzkvc4UZw/featured .

Day 2 ended with an evening presentation of “Cielo”, a documentary film by Alison McAlpine. Highly recommended!

St. Louis, MO – AAS 2019 – Attendees during the Cielo Film Screening at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Tuesday June 11, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

I noted that “Cielo” was presented on the Documentary Channel in Canada. Too bad we do not have a channel like that here in the U.S.!

Day 3 – Wednesday, June 12, 2019
St. Louis, MO – AAS 2019 – Joshua Winn during the Plenary Lecture at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Wednesday June 12, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

Day 3 began with what for me was the finest presentation of the entire conference: Joshua Winn, Princeton University, speaking on “Transiting Exoplanets: Past, Present, and Future”. I first became familiar with Josh Winn through watching his outstanding video course, The Search for Exoplanets: What Astronomers Know, from The Great Courses. I am currently watching his second course, Introduction to Astrophysics, also from The Great Courses. Josh is an excellent teacher, public speaker, and presenter, and it was a great pleasure to meet him at this conference.

Transits provide the richest source of information we have about exoplanets. For example, we can measure the obliquity of the star’s equator relative to the planet’s orbital plane by measuring the apparent Doppler shift of the star’s light throughout transit.

Who was the first to observe a planetary transit? Pierre Gassendi (1592-1655) was the first to observe a transit of Mercury across the Sun in November 1631. Jeremiah Horrocks (1618-1641) was the first to observe a transit of Venus across the Sun in November 1639. Christoph Scheiner (1573-1650) claimed in January 1612 that spots seen moving across the Sun were planets inside Mercury’s orbit transiting the Sun, but we know know of course that sunspots are magnetically cooled regions in the Sun’s photosphere and not orbiting objects at all. Though Scheiner was wrong about the nature of sunspots, his careful observations of them led him to become the first to measure the Sun’s equatorial rotation rate, the first to notice that the Sun rotated more slowly at higher latitudes, and the first to notice that the Sun’s equator is tilted with respect to the ecliptic, and to measure its inclination.

An exoplanet can be seen to transit its host star if the exoplanet’s orbit lies within the transit cone, an angle of 2R*/a centered on our line of sight to the star. R* is the star’s radius, and a is the semi-major axis of the planet’s orbit around the star.

Because of the geometry, we are only able to see transits of 1 out of every 215 Earth-Sun analogs.

Space is by far the best place to study transiting exoplanets.

If an exoplanet crosses a starspot, or a bright spot, on the star, you will see a “blip” in the transit light curve that looks like this:

Transiting exoplanet crossing a starspot (left) or bright spot (right) in the photosphere of the star

Are solar systems like our own rare? Not at all! There are powerful selection effects at work in exoplanet transit statistics. We have discovered a lot of “hot Jupiters” because large, close-in planets are much easier to detect with their short orbital periods and larger transit cones. In actuality, only 1 out of every 200 sun-like stars have hot Jupiters.

Planet statistical properties was the main goal of the Kepler mission. Here are some noteworthy discoveries:

Kepler 89 – two planets transiting at the same time (only known example)

Kepler 36 – chaotic three-body system

Kepler 16 – first known transiting exoplanet in a circumbinary orbit

Transiting Exoplanet Survey Satellite (TESS) – Unlike Kepler, which is in an Earth-trailing heliocentric orbit, TESS is in a highly-elliptical orbit around the Earth with an apogee approximately at the distance of the Moon and a perigee of 108,000 km. TESS orbits the Earth twice during the time the Moon orbits once, a 2:1 orbital resonance with the Moon.

TESS has four 10.5 cm (4-inch) telescopes, each with a 24˚ field of view. Each TESS telescope is constantly monitoring 2300 square degrees of sky.

TESS is fundamentally about short period planets. Data is posted publicly as soon as it is calibrated. TESS has already discovered 700 planet candidates. About 1/2 to 2/3 will be true exoplanets. On average, TESS is observing stars that are about 4 magnitudes brighter than stars observed by Kepler.

The TESS Follow-Up Observing Program (TFOP) is a large working group of astronomical observers brought together to provide follow-up observations to support the TESS Mission’s primary goal of measuring the masses for 50 planets smaller than 4 Earth radii, in addition to organizing and carrying out follow-up of TESS Objects of Interest (TOIs).

HD 21749 – we already had radial velocity data going back several years for this star that hosts an exoplanet that TESS discovered

Gliese 357 – the second closest transiting exoplanet around an M dwarf, after HD 219134

TESS will tell us more about planetary systems around early-type stars.

TESS will discover other transient events, such as supernovae, novae, variable stars, etc. TESS will also make asteroseismology measurements and make photometric measurements of asteroids.

The James Webb Space Telescope (JWST) will be able to do follow-up spectroscopy of planetary atmospheres.

Upcoming exoplanet space missions: CHEOPS, PLATO, and WFIRST.

Hot Jupiter orbits should often be decaying, so this is an important area of study.

Sonification is the process of turning data into sound. For example, you could “listen” to a light curve (with harmonics, e.g. helioseismology and asteroseismology) of a year’s worth a data in just a minute or so.

Solar cycles have different lengths (11-ish years…).

Some predictions: 2019 will be the warmest year on record, 2020 will be less hot. Solar cycle 24 terminate in April 2020. Solar cycle 25 will be weaker than cycle 24. Cycle 25 will start in 2020 and will be the weakest in 300 years, the maximum (such as it is) occurring in 2025. Another informed opinion was that Cycle 25 will be comparable to Cycle 24.

Maunder minimum: 1645 – 1715

Dalton minimum: 1790 – 1820

We are currently in the midst of a modern Gleissberg minimum. It remains to be seen if it will be like the Dalton minimum or a longer “grand minimum” like the Maunder minimum.

Citizen scientists scanning Spitzer Space Telescope images in the Zooniverse Milky Way Project, have discovered over 6,000 “yellow balls”. The round features are not actually yellow, they just appear that way in the infrared Spitzer image color mapping.

Yellow balls (YBs) are sites of 8 solar mass or more star formation, surrounded by ionized hydrogen (H II) gas. YBs thus reveal massive young stars and their birth clouds.

Antlia 2 is a low-surface-brightness (“dark”) dwarf galaxy that crashed into our Milky Way galaxy. Evidence for this collision comes from “galactoseismology” which is the study of ripples in the Milky Way’s disk.

The Large Magellanic Cloud (LMC), Small Magellanic Cloud (SMC), and the Sagittarius Dwarf Galaxy have all affected our Milky Way Galaxy, but galactoseismology has shown that there must be another perturber that has affected the Milky Way. Antlia 2, discovered in November 2018 from data collected by the Gaia spacecraft, appears to be that perturber.

Gaia Data Release 2 (DR2) indicates that the Antlia 2 dwarf galaxy is about 420,000 ly distant, and it is similar in extent to the LMC. It is an ultra-diffuse “giant” dwarf galaxy whose stars average two magnitudes fainter than the LMC. Antlia 2 is located 11˚ from the galactic plane and has a mass around 1010 solar masses.

A question that is outstanding is what is the density of dark matter in Antlia 2? In the future, Antlia 2 may well be an excellent place to probe the nature of dark matter.

Gravity drives the formation of cosmic structure, dark energy slows it down.

Stars are “noise” for observational cosmologists.

“Precision” cosmology needs accuracy also.

The Vera Rubin telescope (Large Synoptic Survey Telescope) in Chile will begin full operations in 2022, collecting 20 TB of data each night!

We have a “galaxy bias” – we need to learn much more about the relation between galaxy populations and matter distribution.

Might there be an irregular asymmetric cycle underlying the regular 22-year sunspot cycle? The dominant period associated with this asymmetry is around 35 to 50 years.

The relationship between differential rotation and constant effective temperature of the Sun: the Sun has strong differential rotation along radial lines, and there is little variation of solar intensity with latitude.

Solar filaments (solar prominences) lie between positive and negative magnetic polarity regions.

Alfvén’s theorem: in a fluid with infinite electric conductivity, the magnetic field is frozen into the fluid and has to move along with it.

Some additional solar terms and concepts to look up and study: field line helicity, filament channels, kinetic energy equation, Lorentz force, magnetic energy equation, magnetic flux, magnetic helicity, magnetohydrodynamics (MHD), meridional flow, polarity inversion lines, relative helicity, sheared arcade, solar dynamo.

Filamentary structures: barbs, Hα, dextral, sinistral.

We would like to be able to predict solar eruptions before they happen.

  1. Magnetic helicity is injected by surface motions.
  2. It accumulates at polarity inversion lines.
  3. It is removed by coronal mass ejections.
Day 4 – Thursday, June 13, 2019

Cahokia (our name for it today) was the largest city north of Mexico 1,000 years ago. It was located at the confluence of the Mississippi, Missouri, and Illinois Rivers. At its height from 1050 – 1200 A.D., Cahokia city covered 6 square miles and had 10,000 to 20,000 people. Cahokia was a walled city. Some lived inside the walls, and others lived outside the walls.

Around 120 mounds were built at greater Cahokia; 70 are currently protected. Platform mounds had buildings on top, and some mounds were used for burial and other uses.

Monks mound is the largest prehistoric earthwork in the Americas. Mound 72 has an appalling history.

Woodhenge – controversial claim that it had an astronomical purpose. Look up Brad Schaefer’s discussion, “Case studies of three of the most famous claimed archaeoastronomical alignments in North America”.

Cahokia’s demise was probably caused by many factors, including depletion of resources and prolonged drought. We do not know who the descendents of the Cahokia people are. It is possible that they died out completely.

The Greeks borrowed many constellations from the Babylonians.

One Sky, Many Astronomies

The neutron skin of a lead nucleus (208Pb) is a useful miniature analog for a neutron star.

Infalling binary neutron stars, such as GW 170817, undergo tidal deformation.

SmallSats

  • Minisatellite: 100-180 kg
  • Microsatellite: 10-100 kg
  • Nanosatellite: 1-10 kg
  • Picosatellite: 0.01-1 kg
  • Femtosatellite: 0.001-0.01 kg

CubeSats are a class of nanosatellites that use a standard size and form factor. The standard CubeSat size uses a “one unit” or “1U” measuring 10 × 10 × 10 cm and is extendable to larger sizes, e.g. 1.5, 2, 3, 6, and even 12U.

The final plenary lecture and the final session of the conference was a truly outstanding presentation by James W. Head III, Brown University, “The Apollo Lunar Exploration Program: Scientific Impact and the Road Ahead”. Head is a geologist who trained the Apollo astronauts for their Moon missions between 1969 and 1972.

St. Louis, MO – AAS 2019 – James Head during the Plenary Lecture at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Thursday June 13, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

During the early years of the space program, the United States was behind the Soviet Union in space technology and accomplishments. The N1 rocket was even going to deliver one or two Soviet cosmonauts to lunar orbit so they could land on the Moon.

Early in his presidency, John F. Kennedy attempted to engage the Soviet Union in space cooperation.

Chris Kraft’s book, Flight: My Life in Mission Control is recommended.

The Apollo astronauts (test pilots) were highly motivated students.

The United States flew 21 robotic precursor missions to the Moon in the eight years before Apollo 11. Rangers 1-9 were the first attempts, but 1 through 6 were failures and we couldn’t even hit the Moon.

Head recommends the recent documentary, Apollo 11, but called First Man Hollywood fiction, saying, “That is not the Neil Armstrong I knew.”

The Apollo 11 lunar samples showed us that the lunar maria (Mare Tranquillitatis) has an age of 3.7 Gyr and has a high titanium abundance.

The Apollo 12 lunar excursion module (LEM) landed about 600 ft. from the Surveyor 3 probe in Oceanus Procellarum, and samples from that mission were used to determine the age of that lunar maria as 3.2 Gyr.

Scientists worked shoulder to shoulder with the engineers during the Apollo program, contributing greatly to its success.

Apollo 11 landed at lunar latitude 0.6˚N, Apollo 12 at 3.0˚S, Apollo 14 at 3.6˚S, and Apollo 15 at 26.1˚N. Higher latitude landings required a plane change and a more complex operation to return the LEM to the Command Module.

The lunar rover was first used on Apollo 15, and allowed the astronauts to travel up to 7 km from the LEM. Head said that Dave Scott did remarkable geological investigations on this mission. He discovered and returned green glass samples, and in 2011 it was determined that there is water inside those beads. Scott also told a little fib to Mission Control to buy him enough time to pick up a rock that turned out to be very important, the “seat belt basalt”.

In speaking about Apollo 16, Head called John Young “one of the smartest astronauts in the Apollo program”.

Harrison Schmitt, Apollo 17, was the only professional geologist to go to the Moon, and he discovered the famous “orange soil”. This is the mission where the astronauts repaired a damaged fender on the lunar rover using duct tape and geological maps to keep them from getting covered in dust while traveling in the rover.

When asked about the newly discovered large mass under the lunar surface, Head replied that it is probably uplifted mantle material rather than an impactor mass underneath the surface.

Radiometric dating of the Apollo lunar samples have errors of about ± 5%.

One of the reasons the Moon’s albedo is low is that space weather has darkened the surface.

The South Pole-Aitken basin is a key landing site for future exploration. In general, both polar regions are of great interest.

Smaller objects like the Moon and Mars cooled efficiently after their formation because of their high surface area to volume ratio.

We do not yet know if early Mars was warm and wet, or cold and icy with warming episodes. The latter is more likely if our solar system had a faint young sun.

Venus has been resurfaced in the past 0.5 Gyr, and there is no evidence of plate tectonics. The first ~80% of the history of Venus is unknown. Venus probably had an ocean and tectonic activity early on, perhaps even plate tectonics. Venus may have undergone a density inversion which exchanged massive amounts of material between the crust and mantle. 80% of the surface of Venus today is covered by lava flows.

A mention was made that a new journal of Planetary Science (in addition to Icarus, presumably) will be coming from the AAS soon.

St. Louis, MO – AAS 2019 – Attendees during the Donors, Sponsors, and 40+E Reception at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Wednesday June 12, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.
St. Louis, MO – AAS 2019 – Attendees during the Donors, Sponsors, and 40+E Reception at the American Astronomical Society’s 234th meeting at the Saint Louis Union Station Hotel in St. Louis, Missouri, Wednesday June 12, 2019. The AAS, established in 1899 and based in Washington, DC, is the major organization of professional astronomers in North America. More than 500 astronomers, educators, industry representatives, and journalists are spending the week in St. Louis to discuss the latest findings from across the universe. Photo by Phil McCarten, © 2019 AAS/CorporateEventImages.

I attend a lot of meetings and lectures (both for astronomy and SAS), and I find that I am one of the few people in attendance who write down any notes. Granted, a few are typing at their devices, but one never knows if they are multitasking instead. For those that don’t take any notes, I wonder, how do they really remember much of what they heard days or weeks later without having written down a few keywords and phrases and then reviewing them soon after? I did see a writer from Astronomy Magazine at one of the press conferences writing notes in a notebook as I do. I believe it was Jake Parks.

Anyone who knows me very well knows that I love traveling by train. To attend the AAS meeting, I took a Van Galder bus from Madison to Chicago, and then Amtrak from Chicago to St. Louis. Pretty convenient that the AAS meeting was held at the Union Station Hotel, just a few blocks from Amtrak’s Gateway Station. It is a fine hotel with a lot of history, and has an excellent on-site restaurant. I highly recommend this hotel as a place to stay and as a conference venue.

The bus and train ride to and fro afforded me a great opportunity to catch up on some reading. Here are a few things worth sharing.

astrometry.net – you can upload your astronomical image and get back an image with all the objects in the image astrometrically annotated. Wow!

16 Psyche, the most massive metal-rich asteroid, is the destination for a NASA orbiter mission that is scheduled to launch in 2022 and arrive at Psyche in 2026. See my note about 16 Psyche in the AAS notes above.

The lowest hourly meteor rate for the northern hemisphere occurs at the end of March right after the vernal equinox.

A tremendous, dynamic web-based lunar map is the Lunar Reconnaissance Orbiter Camera (LROC) Quickmap, quickmap.lroc.asu.edu.

I read with great interest Dr. Ken Wishaw’s article on pp. 34-38 in the July 2019 issue of Sky & Telescope, “Red Light Field Test”. Orange or amber light is probably better that red light for seeing well in the dark while preserving your night vision. You can read his full report here. Also, see my article “Yellow LED Astronomy Flashlights” here.

Jupiter and Saturn will have a spectacular conjunction next year. As evening twilight fades on Monday, December 21, 2020, the two planets will be just 1/10th of a degree apart, low in the southwestern sky.

An oblate spheroid with axes a = b > c is called a Maclaurin spheroid. If all three axes have different lengths a > b > c, then you have a Jacobi ellipsoid.

The light curve of a stellar occultation by a minor planet (asteroid or TNO) resembles a square well if the object has no atmosphere (or one so thin that it cannot be detected, given the sampling rate and S/N), and the effects of Fresnel diffraction and the star’s angular diameter are negligible.

Astronomer Margaret Burbidge, who turns 100 on August 12, 2019, refused the AAS Annie Jump Cannon Award in 1972, stating in her rejection letter that “it is high time that discrimination in favor of, as well as against, women in professional life be removed, and a prize restricted to women is in this category.” In 1976, Margaret Burbidge became the first woman president of the AAS, and in 1978 she announced that the AAS would no longer hold meetings in the states that had not ratified the Equal Rights Amendment (ERA).

During the days following the conference when I was writing this report, I received the happy news from both the AAS and Sky & Telescope that AAS was the winning bidder of S&T during a bankruptcy auction of its parent company, F+W Media. I believe that this partnership between the AAS and Sky & Telescope will benefit both AAS members and S&T readers immensely. Peter Tyson, Editor in Chief of Sky & Telescope, stated in the mutual press release, “It feels like S&T is finally landing where it belongs.” I couldn’t agree more!