Majriti (exoplanet)
Exoplanet Majriti |
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Artist's impression of Majriti with hypothetical companions, viewed from above a hypothetical earth-like exomoon | |
Constellation | Andromeda |
Position equinox : J2000.0 |
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Right ascension | 01h 36m 47.843s |
declination | + 41 ° 24 ′ 19.65 ″ |
Orbit data | |
Central star | Titawin A |
Major semi-axis | 2.51329 ± 0.00075 AU |
eccentricity | 0.2987 ± 0.0072 |
Period of circulation | 1276.46 ± 0.57 d |
Further data | |
Minimum dimensions | 4,132 ± 0.029 M J |
distance | 13.57 ± 0.02 pc |
history | |
discovery | Marcy et al. |
Date of discovery | 1999 |
Catalog names | |
υ And d, 50 And d, HR 458 d, GJ 61 d, HD 9826 d |
Majriti ( Upsilon Andromedae d , also abbreviated υ And d ) is an exoplanet that the approximately 44.25 light years from the sun distant main sequence star Titawin A in the binary system Titawin ( Upsilon Andromedae ) in the constellation Andromeda orbits. It is one of four known planets in the star's planetary system .
Origin of name
Like all exoplanets, Majriti was originally designated with the star's official name and a lowercase letter, according to the order in which it was discovered. After a publicly advertised competition by the IAU , on December 15, 2015, it was given an official name after Maslama al-Majriti (i.e. 'from Madrid ', 'the Madrid'), an Arab astronomer of the 10th and early 11th centuries in al-Andalus .
discovery
After the discovery of the first planet ( Saffar ) in 1996, further investigations of the star with an Échelle spectrograph took place. Astronomers from San Francisco State University and the Harvard-Smithsonian Center for Astrophysics independently concluded that a planetary system with three planets would most closely match the measurements. The two newly announced planets were named Ypsilon Andromedae c and Ypsilon Andromedae d.
properties
Majriti orbits its central star approximately every 1276.46 days, whereby its orbit, like that of the further inward orbiting planet υ And c, is very eccentric . It has a large orbit half-axis of a little more than 2.5 AU . Apart from its high orbital eccentricity (greater than that of the dwarf planet Pluto ), υ And d also has a significant orbital inclination compared to υ And c, which is mutually 30 °.
The minimum mass of the planet is a little more than four masses of Jupiter . The actual mass could be 10.25 Jupiter's masses. Due to its mass, it is very likely that it is a gas planet . Its atmosphere could have clouds of water. Majriti is in the habitable zone of its central star, so that life-friendly conditions could possibly prevail on a moon orbiting it.
Individual evidence
- ↑ VizieR: HIP 7513. Retrieved May 19, 2015 .
- ↑ a b c d NASA Exoplanet Archive: ups And d. Retrieved May 19, 2015 .
- ↑ International Astronomical Union: NameExoWorlds - The Approved Names. Retrieved January 3, 2016 .
- ^ Butler, R. Paul et al .: Evidence for Multiple Companions to υ Andromedae . bibcode : 1999ApJ ... 526..916B .
- ^ Curiel, S. et al .: A fourth planet orbiting υ Andromedae . bibcode : 2011A & A ... 525A..78C .
- ^ A b McArthur, Barbara E. et al .: New Observational Constraints on the υ Andromedae System with Data from the Hubble Space Telescope and Hobby-Eberly Telescope . bibcode : 2010ApJ ... 715.1203M .
- ↑ Sudarsky, David et al .: Theoretical Spectra and Atmospheres of Extrasolar Giant Planets . arxiv : astro-ph / 0210216 .
- ↑ Buccino, Andrea P. et al .: Ultraviolet Radiation Constraints around the Circumstellar Habitable Zones . arxiv : astro-ph / 0512291 .