Classical Music Timeline: 1840s

This is one of a series of postings of important classical music dates, from the 17th century to the present. Included are the date and location of the birth and death of composers, and the premiere date and location of the first public performance of works. When the premiere date and location is unknown, the date or year of completion of the work is given. Though reasonably comprehensive, this is a subjective list, so the choice of composers and works is mine. If you find any errors, or if you can offer a premiere date and location for a work where only the completion date or year is listed, please post a comment here.

1840
May 7 – Pyotr Ilyich Tchaikovsky (1840-1893) was born in Votkinsk, Russia

September 30 – Johan Svendsen (1840-1911) was born in Oslo, Norway

1841
January 18 – Emmanuel Chabrier (1841-1894) was born in Ambert, France

March 31 – Symphony No. 1 in B♭ major, op. 38, “Spring”, by Robert Schumann (1810-1856) was first performed in Leipzig, Germany

September 8 – Antonín Dvořák (1841-1904) was born in Nelahozeves, Czech Republic

October 17 – Symphony No. 5 in B♭ major, D. 485, by Franz Schubert (1797-1828) was first performed in Vienna, Austria

December 6 – The 1st version of Symphony No. 4 in D minor, op. 120 (much preferred by Johannes Brahms) by Robert Schumann (1810-1856) was first performed in Leipzig, Germany

1842
Louise Farrenc (1804-1875) completed Symphony No. 1 in C minor, op. 32

March 3 – Symphony No. 3 in A minor, op. 56, “Scottish”, by Felix Mendelssohn (1809-1847) was first performed in Leipzig, Germany

March 9 – Sinfonia from the opera Nabucco by Giuseppe Verdi (1813-1901) was first performed in Milan, Italy

May 12 – Jules Massenet (1842-1912) was born in Saint-Étienne, France

December 9Ruslan and Lyudmila, opera by Mikhail Glinka (1804-1857), was first performed in Saint Petersburg, Russia

1843
January 8 – Piano Quintet in E♭ major, op. 44 by Robert Schumann (1810-1856) was first performed in Leipzig, Germany

June 15 – Edvard Grieg (1843-1907) was born in Bergen, Norway

1844
Frédéric Chopin (1810-1849) completed Piano Sonata No. 3 in B minor, op. 58

February 21 – Charles-Marie Widor (1844-1937) was born in Lyon, France

March 10 – Pablo de Sarasate (1844-1908) was born in Pamplona, Spain

March 18 – Nikolai Rimsky-Korsakov (1844-1908) was born in Tikhvin, Russia

1845
Charles Auguste de Bériot (1802-1870) completed the Violin Concerto No. 8 in D major, op. 99

Mikhail Glinka (1804-1857) completed Capriccio brillante on the Jota aragonesa, Spanish Overture No. 1

March 13 – Violin Concerto in E minor, op. 64, by Felix Mendelssohn (1809-1847) was first performed in Leipzig, Germany

May 12 – Gabriel Fauré (1845-1924) was born in Pamiers, France

December 4 – Piano Concerto in A minor, op. 54 by Robert Schumann (1810-1856) was first performed in Dresden, Germany

1846
November 5 – Symphony No. 2 in C major, op. 61 by Robert Schumann (1810-1856) was first performed in Leipzig, Germany

1847
Louise Farrenc (1804-1875) completed Symphony No. 3 in G minor, op. 36

Frédéric Chopin (1810-1849) completed Waltz in C♯ minor, op. 64, no. 2

November 4 – Felix Mendelssohn (1809-1847) died in Leipzig, Germany

1849
Robert Schumann (1810-1856) completed the Romances and Ballads, op. 75, for SATB choir a cappella

March – Robert Schumann (1810-1856) completed the Romances, op. 69, for female voices (SSAA) a cappella

March – Robert Schumann (1810-1856) completed the Romances, op. 91, for female SSAA choir a cappella

October 17 – Frédéric Chopin (1810-1849) died in Paris, France

November 19 – Symphony No. 4 in C minor, D. 417, “Tragic”, by Franz Schubert (1797-1828) was first performed in Leipzig, Germany

December 8 – Sinfonia from the opera Luisa Miller by Giuseppe Verdi (1813-1901) was first performed in Naples, Italy

1830s

1850s

Spectroscopic Parallax

For the nearest stars, the change in the position of the Earth in its orbit results in a tiny shift in the position of the nearby star relative to the distant background stars. This shift is called the trigonometric parallax. You can see the effect by holding your thumb up at arms length, closing your left eye, and lining up your thumb with something across the room. Now, alternate back and forth between having your right eye open and your left eye open and you’ll see the position of your thumb shift relative to an object further away. Move your thumb closer, and the shift is larger. That is the essence of trigonometric parallax.

Trigonometric Parallax

The distance to the star in parsecs (1 pc = 3.26 ly) is just

Now, a star’s distance, apparent brightness, and “true” (or intrinsic) brightness are related in the following way:

M = m + 5 (1 – log d)

where M = the absolute magnitude of the star

and m = the apparent magnitude of the star

and d = the distance to the star in parsecs

The absolute magnitude is the apparent magnitude the star would have if it were at a distance of 10 parsecs. Looking at it another way, the absolute magnitude is a proxy for the intrinsic brightness. The apparent magnitude is the star’s apparent brightness (as seen from Earth).

While the above equation is highly useful for general purpose calculations, to get the most accurate values astronomers must take into account atmospheric and interstellar extinction. And, anytime we deal with a star’s luminosity and its apparent brightness at some distance, d , we must specify the photometric system and optical filter that is being used. Or, less commonly (for practical reasons), we specify that the star’s luminosity and apparent brightness is to include all wavelengths of the electromagnetic spectrum, thus bolometric magnitudes are to be used.

Spectroscopic parallax is a bit of a misnomer, but here’s how it works for approximating the distance to main-sequence stars that are too far away to exhibit a measurable, reasonably certain, trigonometric parallax: measure the apparent magnitude of the star, and then using its spectrum to find its position on the H-R diagram, read off its absolute magnitude. Using your measured apparent magnitude and the star’s estimated absolute magnitude, you can solve for d the distance in the above equation.

Hertzsprung–Russell (H-R) diagram

The star’s color (the x-axis on the H-R diagram) is easy to measure, but a deeper analysis of the spectral lines is needed to determine whether the star is a main-sequence, giant, or supergiant star (or something else).