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HD 28185 b is an extrasolar planet 128 light-years away from Earth in the constellation of Eridanus. The planet was discovered orbiting the Sun-like star HD 28185 in April 2001 as a part of the CORALIE survey for southern extrasolar planets, and its existence was independently confirmed by the Magellan Planet Search Survey in 2008.[3] HD 28185 b orbits its sun in a circular orbit that is at the inner edge of its star's habitable zone.[4]

HD 28185 b
An artist's impression of HD28185 b
Discovery
Discovered bySantos et al.
Discovery siteLa Silla Observatory
Discovery dateApril 4, 2001[1]
Detection method
Radial velocity (CORALIE)
Orbital characteristics[2]
Semi-major axis
1.035+0.042
−0.046 AU
Eccentricity0.055+0.004
−0.003
Orbital period (sidereal)
1.056 ± 0.0002 years (385.704 ± 0.073 d)
Time of periastron
2452262.394+3.714
−3.315
Argument of periastron
356.596°+3.495°
−3.155°
Semi-amplitude163.657+0.653
−0.533
StarHD 28185
Physical characteristics[2]
Mass≥5.837+0.486
−0.510 MJ

    Discovery


    HD 28185 b was discovered by detecting small periodic variations in the radial velocity of its parent star caused by the gravitational attraction of the planet. This was achieved by measuring the Doppler shift of the star's spectrum. In 2001 it was announced that HD 28185 exhibited a wobble along the line-of-sight with a period of 383 days, with an amplitude indicating a minimum mass 5.72 times that of Jupiter.[1][5]


    Orbit and mass


    HD 28185 b takes 1.04 years to orbit its parent star. Unlike most known long-period planets, the orbit of HD 28185 b has a low eccentricity, comparable to that of Mars in the Solar System.[6] The orbit lies entirely within its star's habitable zone.[4]

    The amplitude of the radial velocity oscillations means that the planet has a mass at least 5.7 times that of Jupiter in the Solar System. However, the radial velocity method only yields a minimum value on the planet's mass, depending on the orbital inclination to our line-of-sight. Therefore, the true mass of the planet may be much greater than this lower limit.


    Characteristics


    Given the planet's high mass, it is most likely to be a gas giant with no solid surface. Since the planet has only been detected indirectly through observations of the star, properties such as its radius, composition, and temperature are unknown. Periastron (0.959 AU), semimajor axis (1.031 AU) and apastron (1.102 AU) irradiances are 112%, 96.6% and 84.5% that of the Earth. [note 1]

    Since HD 28185 b orbits in its star's habitable zone, some have speculated on the possibility of life on worlds in the HD 28185 system.[7] While it is unknown whether gas giants can support life, simulations of tidal interactions suggest that HD 28185 b could harbor Earth-mass satellites in orbit around it for many billions of years.[8] Such moons, if they exist, may be able to provide a habitable environment, though it is unclear whether such satellites would form in the first place.[9] Additionally, a small planet in one of the gas giant's Trojan points could survive in a habitable orbit for long periods.[10] The high mass of HD 28185 b, of over six Jupiter masses, actually makes either of these scenarios more likely than if the planet was about Jupiter's mass or less.


    See also



    Notes


    1. From Star radius is 1.15 times solar, temperature is 5609 K compared to the sun 5777 K. Irradiance is given by bolometric luminosity divided by square of distance, flux divided by Solar Constant, ratio relative to Earth.

    References


    1. "Exoplanets: The Hunt Continues!" (Press release). Garching, Germany: European Southern Observatory. April 4, 2001. Retrieved December 27, 2012.
    2. Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21). arXiv:2208.12720. Bibcode:2022arXiv220812720F. doi:10.3847/1538-4365/ac7e57.
    3. Minniti, Dante; et al. (2009). "Low-Mass Companions for Five Solar-Type Stars From the Magellan Planet Search Program". The Astrophysical Journal. 693 (2): 1424–1430. arXiv:0810.5348. Bibcode:2009ApJ...693.1424M. doi:10.1088/0004-637X/693/2/1424.
    4. Jones, Barrie W.; Sleep, P. Nick; Underwood, David R. (2006). "Habitability of Known Exoplanetary Systems Based on Measured Stellar Properties". The Astrophysical Journal. 649 (2): 1010–1019. arXiv:astro-ph/0603200. Bibcode:2006ApJ...649.1010J. doi:10.1086/506557.
    5. Santos, N.; et al. (2001). "The CORALIE survey for southern extra-solar planets VI. New long-period giant planets around HD 28185 and HD 213240". Astronomy and Astrophysics. 379 (3): 999–1004. arXiv:astro-ph/0106255. Bibcode:2001A&A...379..999S. doi:10.1051/0004-6361:20011366. Archived from the original on 2006-07-13.
    6. Butler, R. P.; et al. (2006). "Catalog of Nearby Exoplanets". The Astrophysical Journal. 646 (1): 505–522. arXiv:astro-ph/0607493. Bibcode:2006ApJ...646..505B. doi:10.1086/504701.
    7. Mullen, L. (2001). "Extrasolar Planets with Earth-like Orbits". Archived from the original on 29 September 2006. Retrieved 22 July 2006.
    8. Barnes, J., O'Brien, D. (2002). "Stability of Satellites around Close-in Extrasolar Giant Planets". Astrophysical Journal. 575 (2): 1087–1093. arXiv:astro-ph/0205035. Bibcode:2002ApJ...575.1087B. doi:10.1086/341477.{{cite journal}}: CS1 maint: multiple names: authors list (link)
    9. Canup, R.; Ward, W. (2006). "A common mass scaling for satellite systems of gaseous planets". Nature. 441 (7095): 834–839. Bibcode:2006Natur.441..834C. doi:10.1038/nature04860. PMID 16778883.
    10. Schwarz, R.; Dvorak, R.; Süli, Á.; Érdi, B. (2007). "Survey of the stability region of hypothetical habitable Trojan planets". Astronomy and Astrophysics. 474 (3): 1023–1029. Bibcode:2007A&A...474.1023S. doi:10.1051/0004-6361:20077994.


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    На других языках

    [de] HD 28185 b

    HD 28185 b ist ein Exoplanet, der den gelben Zwerg HD 28185 umkreist. Auf Grund seiner hohen Masse wird angenommen, dass es sich um einen Gasplaneten handelt.
    - [en] HD 28185 b

    [es] HD 28185 b

    HD 28185 b es un planeta extrasolar aproximadamente a 138 años luz de la Tierra en la constelación de Eridanus. El planeta fue descubierto en órbita alrededor de la estrella HD 28185 como el Sol. en abril de 2001 como parte de la encuesta CORALIE para el sur de planetas extrasolares y su existencia fue confirmada de manera independiente por el Magallanes Planet Search Survey en 2008.[1] HD 28185 b orbita su estrella en una trayectoria circular que está en el borde interior de la zona habitable de su estrella.[2]

    [ru] HD 28185 b

    HD 28185 b — экзопланета, расположенная на расстоянии 128,6 св. лет от Земли в южном созвездии Эридана.


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