C / 1590 E1
| C / 1590 E1 [i] | |
|---|---|
| Properties of the orbit ( animation ) | |
| Orbit type | parabolic |
| Numerical eccentricity | 1.0 |
| Perihelion | 0.568 AU |
| Inclination of the orbit plane | 150.5 ° |
| Perihelion | February 8, 1590 |
| Orbital velocity in the perihelion | 55.9 km / s |
| history | |
| Explorer | Tycho Brahe et al. a. |
| Date of discovery | March 5, 1590 |
| Older name | 1590 |
| Source: Unless otherwise stated, the data comes from JPL Small-Body Database Browser . Please also note the note on comet articles . | |
C / 1590 E1 is a comet that could be seen with the naked eye in 1590 .
Discovery and observation
From March 5th to 17th, 1590 (dates in the greg. Calendar ) a comet of medium brightness could be observed. It had a long tail that pointed to the zenith and moved rapidly across the sky. He was discovered by several people, the most notable among them was Tycho Brahe , who him from his observatory Uraniborg watched and left as with the previously observed by him comet comprehensive record of it.
On the evening of March 5, the comet appeared with the brightness of a star of the 2nd magnitude, the tail had a length of 4–5 ° . That same night the brightness increased slowly to that of a star of the first magnitude and the tail reached 7 ° longitude. On further observations, Brahe was able to determine that the tail always pointed away from the sun .
The tail was no longer visible until March 12, and on March 16 the comet only appeared with a round coma . This indicates that the originally rather inconspicuous comet only experienced an outbreak of brightness shortly before its discovery and quickly faded a few days later.
Scientific evaluation
Tycho Brahe was already able to calculate an ephemeris of the comet from his observations . A manuscript with the calculation of an ephemeris has also survived from Jacques de Billy from Dijon . The first, the determination of the of Brahe's observation data path elements could make was Edmond Halley . Later in the 19th century a new calculation was made by John Russell Hind . These values are given in the info box.
Orbit
Due to the uncertain observation data, only a parabolic orbit could be determined for the comet , which is inclined by around 150 ° to the ecliptic . It thus runs in the opposite direction (retrograde) like the planets through its orbit. At the point of the orbit closest to the sun ( perihelion ), which the comet passed on February 8, 1590, it was located at a distance of 84.9 million km from the sun in the area between the orbits of Mercury and Venus . As early as November 19, 1589, it had passed Mars at a distance of about 57.5 million km and on January 29, 1590 it had approached Mercury to about 42.5 million km. On March 3, Earth came unusually close to within approximately 0.25 AU / 37.1 million km, which was the reason for its observed brightness and rapid movement across the sky. On March 14th, Venus was passed at a distance of about 41.7 million km.
By passing relatively close to Saturn on October 9, 1586 and April 25, 1591 at a distance of just over 5 AU, as well as at Jupiter on February 27, 1590 in a distance of slightly less than 5 AU, the eccentricity of the comet's orbit tended to increase even further . Due to the uncertain initial data, however, no definitive statement can be made as to whether the orbit became hyperbolic as a result or whether the comet could return to the inner solar system .
The orbital elements of the comet of 1590 are significantly similar to those of comet C / 1992 J2 (Bradfield) . They could both have a common origin.
See also
Web links
Individual evidence
- ^ AG Pingré: Cométographie ou Traité historique et théorique des comètes. Tome I, Paris 1783, pp. 554-556.
- ^ DWE Green: Assessment of Early-Modern Observations of Comets and Supernovae: Focus on Pre-Telescopic European Astrometric and Physical Data. Thesis, Durham University, Durham 2004, pp. 202-203 ( PDF; 13.52 MB ).
- ^ R. Wielen, Thomas Hockey (Ed.): Bibliographical Encyclopedia of Astronomers. Springer, New York 2007, ISBN 978-0-387-31022-0 , p. 125.
- ↑ C / 1590 E1 in the Small-Body Database of the Jet Propulsion Laboratory (English).
- ↑ A. Vitagliano: SOLEX 11.0. Archived from the original on September 18, 2015 ; accessed on May 2, 2014 .
- ↑ L. Neslušan and M. Jakubík: The tidal action of the homogeneous field of Galactic-disc matter and population of the outer Oort cloud. In: Contributions of the Astronomical Observatory Skalnaté Pleso. Vol. 34, 2004, pp. 87-104 ( bibcode : 2004CoSka..34 ... 87N ).