Aldebaran b

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Aldebaran b
Discovery
Discovery date1993 (dubious)
May 15, 2015 (confirmed)
2019 (dubious, again)
Radial velocity
Orbital characteristics
Apastron 1.606 +0.2105
−0.2375 AU
Periastron 1.314 +0.3295
−0.3025 AU
1.46 ± 0.27 AU (218,000,000 ± 40,000,000 km)
Eccentricity 0.1 ± 0.05
628.96 ± 0.9 d
1999/04/28 ± 50
287 ± 29
Star Aldebaran
Physical characteristics
Mass >5.8±0.7 [1] MJ
Temperature 1,500 K (1,230 °C; 2,240 °F)

    Aldebaran b is a candidate exoplanet orbiting the orange giant star Aldebaran, 65 light-years away. It was initially detected in 1993, but was considered doubtful until 2015, when researchers came to a conclusion that there is likely an exoplanet orbiting Aldebaran, consistent with the original calculations, but also compatible with stellar activity. [2] However, in 2019, new data placed doubts on its existence again. [3]

    Contents

    Physical properties

    Mass and orbit

    Aldebaran b is a giant exoplanet with at least 5.8 times the mass of Jupiter. It orbits at a distance about 45% farther than Earth does from the Sun. The equilibrium temperature of this planet is likely to be around 1,500 K (1,230 °C; 2,240 °F), as it is strongly irradiated by its giant host star. Nevertheless, when Aldebaran was a main sequence star, it is likely that the planet had an equilibrium temperature comparable to that of the Earth. [1]

    Host star

    The host star, Aldebaran, is an orange giant star, meaning it has moved off from the main sequence and exhausted the supply of hydrogen in the core. It has a spectral class of K5 III. [4]

    Aldebaran is a K-type star that is 1.16 ± 0.07 times the mass [1] and 44 times the radius of the Sun. It has a surface temperature of 3,910 K. In comparison, the Sun has a surface temperature of 5778 K. [5]

    The star's average apparent magnitude, or how bright it usually appears from Earth, is 0.86, easily visible to the naked eye.

    Discovery

    1993 proposal

    The exoplanet was first proposed in 1993, radial velocity measurements of Aldebaran, Arcturus and Pollux showed that Aldebaran exhibited a long-period radial velocity oscillation, which could be interpreted as a substellar companion. The measurements for Aldebaran implied a companion with a minimum mass 11.4 times that of Jupiter in a 643-day orbit at a separation of 2.0 AU (300 Gm) in a mildly eccentric orbit. However, all three stars surveyed showed similar oscillations yielding similar companion masses, and the authors concluded that the variation was likely to be intrinsic to the star rather than due to the gravitational effect of a companion. [6]

    2015 confirmed status

    In 2015, a study showed stable long-term evidence for both a planetary companion and stellar activity. [7]

    2019 doubts on existence

    In 2019, an analysis of additional data provided by Lick Observatory has placed the existence of Aldebaran b in serious doubt, because of apparent phase jitter of radial-velocity signal; a better data fit is obtained by either two planets or no planets at all around Aldebaran. [3]

    See also

    Related Research Articles

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    References

    1. 1 2 3 Farr, W. (2018). "Aldebaran b's temperate past uncovered in planet search data". The Astrophysical Journal. 865 (2): L20. arXiv: 1802.09812 . Bibcode:2018ApJ...865L..20F. doi: 10.3847/2041-8213/aadfde . S2CID   56049041.
    2. ↑ Hatzes, A.P.; et al. (May 15, 2015). "Long-lived, long-period radial velocity variations in Aldebaran: A planetary companion and stellar activity". Astronomy & Astrophysics. 580: 18. arXiv: 1505.03454 . Bibcode:2015yCat..35800031H. doi:10.1051/0004-6361/201425519. S2CID   53324086.
    3. 1 2 Reichert, Katja (March 25, 2019). "Precise radial velocities of giant stars XII. Evidence against the proposed planet Aldebaran b". Astronomy & Astrophysics. A22: 625. arXiv: 1903.09157 . Bibcode:2019A&A...625A..22R. doi:10.1051/0004-6361/201834028. S2CID   85459692.
    4. ↑ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv: astro-ph/0603770 . Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID   119476992.
    5. ↑ Fraser Cain (September 15, 2008). "Temperature of the Sun". Universe Today . Retrieved February 19, 2011.
    6. ↑ Hatzes, A.; Cochran, W. (1993). "Long-period radial velocity variations in three K giants". The Astrophysical Journal . 413 (1): 339–348. Bibcode:1993ApJ...413..339H. doi: 10.1086/173002 .
    7. ↑ Hatzes, A. P.; Cochran, W. D.; et al. (2015). "Long-lived, long-period radial velocity variations in Aldebaran: A planetary companion and stellar activity". Astronomy & Astrophysics. 580: A31. arXiv: 1505.03454 . Bibcode:2015A&A...580A..31H. doi:10.1051/0004-6361/201425519. S2CID   53324086.
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