Majriti (exoplanet)

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Exoplanet
Majriti

Artist's impression of Majriti with hypothetical companions, viewed from above a hypothetical earth-like exomoon

Artist's impression of Majriti with hypothetical companions, viewed from above a hypothetical earth-like exomoon
Constellation Andromeda
Position
equinox : J2000.0
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

  1. ↑ VizieR: HIP 7513. Retrieved May 19, 2015 .
  2. ↑ a b c d NASA Exoplanet Archive: ups And d. Retrieved May 19, 2015 .
  3. ↑ International Astronomical Union: NameExoWorlds - The Approved Names. Retrieved January 3, 2016 .
  4. ^ Butler, R. Paul et al .: Evidence for Multiple Companions to υ Andromedae . bibcode : 1999ApJ ... 526..916B .
  5. ^ Curiel, S. et al .: A fourth planet orbiting υ Andromedae . bibcode : 2011A & A ... 525A..78C .
  6. ^ 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 .
  7. ↑ Sudarsky, David et al .: Theoretical Spectra and Atmospheres of Extrasolar Giant Planets . arxiv : astro-ph / 0210216 .
  8. ↑ Buccino, Andrea P. et al .: Ultraviolet Radiation Constraints around the Circumstellar Habitable Zones . arxiv : astro-ph / 0512291 .