HD 86081

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HIP 86081 / Bibhā
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Sextans
Right ascension 09h 56m 05.91853s [1]
Declination −03° 48′ 30.3233″ [1]
Apparent magnitude  (V)8.73 [2]
Characteristics
Spectral type G1V [3]
B−V color index 0.664±0.026 [2]
Astrometry
Radial velocity (Rv)+30.88±0.27 [2]  km/s
Proper motion (μ)RA: −67.001±0.079 [1]   mas/yr
Dec.: 15.999±0.076 [1]   mas/yr
Parallax (π)9.5928 ± 0.0509  mas [1]
Distance 340 ± 2  ly
(104.2 ± 0.6  pc)
Absolute magnitude  (MV)3.86 [2]
Details [4]
Mass 1.21±0.28  M☉
Radius 1.46±0.14  R☉
Luminosity 2.941 [1]   L☉
Surface gravity (log g)4.25 [5]   cgs
Temperature 5,973 [1]   K
Metallicity [Fe/H]+0.22  dex
Rotational velocity (v sin i)5.0 [5]  km/s
Age 3.61±0.86  Gyr
Other designations
Bibhā, BD−03 2815, HD  86081, HIP  48711, SAO  137236 [6]
Database references
SIMBAD data

HD 86081 is a yellow-hued star in the equatorial constellation of Sextans. It has the proper name Bibhā, the Bengali form of a Sanskrit word meaning a bright beam of light. [7] The star is named after the physicist Bibha Chowdhuri (1913-1991), who studied cosmic rays.[ citation needed ] This name was suggested in the 2019 NameExoWorlds campaign. [7] With an apparent visual magnitude of 8.73, [2] this star is too dim to be viewed with the naked eye but can be seen with a small telescope. It is located at a distance of approximately 340  light years from the Sun based on parallax, and is drifting further away with a radial velocity of +31 km/s. [2]

Contents

Characteristics

The stellar classification of this star is G1V, [3] which indicates this is a G-type main-sequence star that, like the Sun, is generating energy through hydrogen fusion at its core. It is bigger and more massive than the Sun at 1.46 and 1.21 solar units respectively. The star is an estimated 3.6 [4]  billion years old and is spinning with a projected rotational velocity of 5 km/s. [5] It is chromospherically inactive, with no emission seen in the core of the Ca II H and K lines. [8] HD 86081 is radiating 2.9 [1] times the luminosity of the Sun from its photosphere at an effective temperature of 5,973 K. [1]

Planetary system

Monitoring of this star for radial velocity variations began in November 2005 and the first companion was discovered on April 17, 2006. [8] This hot Jupiter is orbiting just 5,180,000 km from the host star and has an orbital period of 2.1 days, one of the shortest periods ever discovered by this technique. [4] The separation of this exoplant is sufficiently low that it may have sped up the star's rotation through tidal interaction. [9] HD 86081 shows no evidence of planetary transits in spite of a 17.6% transit probability. [8] There is a linear trend in the star's radial velocity measurements that may be an indicator of additional unseen companions. [4]

The HD 86081 planetary system [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Santamasa ≥1.48±0.23  MJ 0.0346±0.00272.1378431±0.00000310.0119±0.0047——

See also

Related Research Articles

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HD 224693, also named Axólotl, is a star in the equatorial constellation of Cetus, and is positioned near the western constellation border with Aquarius. It can be viewed with a small telescope but is too faint to be seen with the naked eye, having an apparent visual magnitude of 8.23. Based on parallax measurements, the object is located at a distance of approximately 306 light years from the Sun. It is drifting further away with a radial velocity of 1.5 km/s.

HD 170469 is a probable binary star system in the equatorial constellation of Ophiuchus. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.21. The system is located at a distance of 197 light years away from the Sun based on parallax. It is drifting closer with a radial velocity of −59 km/s, and is expected to come to within 49.8 light-years in about 959,000 years.

HD 17156, named Nushagak by the IAU, is a yellow subgiant star approximately 255 light-years away in the constellation of Cassiopeia. The apparent magnitude is 8.17, which means it is not visible to the naked eye but can be seen with good binoculars. A search for a binary companion star using adaptive optics at the MMT Observatory was negative.

HD 43691 is a star with an orbiting exoplanet in the constellation Auriga. With an apparent visual magnitude of 8.03, it is too faint to be visible to the naked eye. This system is located at a distance of 279 light years based on parallax measurements, but is drifting closer with a heliocentric radial velocity of −29 km/s.

HD 231701 is a yellow-white hued star in the northern constellation of Sagitta, near the southern constellation border with Aquila. With an apparent visual magnitude of 8.97, it is too dim to be viewed with the naked eye, but can be seen with powerful binoculars or a small telescope. Parallax measurements provide a distance estimate of approximately 356 light years from the Sun, but it is drifting closer with a radial velocity of −63 km/s. It is predicted to come as close as 189.5 light-years in 1.345 million years.

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HD 86081 b or Santamasa, meaning 'clouded' in Sanskrit, is a gas giant exoplanet that orbits close to its host star HD 86081 or Bibha, completing its orbit in only 2.1375 days. With such a short orbit it belongs to the class of exoplanets known as hot Jupiters. Like most Hot Jupiters, the orbit is nearly circular, with an eccentricity of 0.008. On 17 December 2019, the International Astronomical Union, Paris has selected the name 'Santamasa' suggested by 13 year old Vidyasagar Daud, class 8th student of Sinhgad Spring Dale Public School, Pune, India for the exoplanet HD 86081 b. This large scale election procedure has come up across India. The name echoes the Indian sentiments through the name 'Sant' (संत), 'Tamas' (तमस्) refers to "darkness", similarly the entire name 'Santamasa' matched with the characteristics of the exoplanet being clouded.

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HD 179079 is a star with an exoplanetary companion in the equatorial constellation of Aquila. It has an apparent visual magnitude of approximately 7.96, making it too faint to be readily visible to the naked eye. The distance to this star can be determine using parallax measurements, which yields an estimate of approximately 228 light years. It is drifting further away with a radial velocity of +20 km/s.

<span class="mw-page-title-main">HD 15082</span> Star in the constellation Andromeda

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References

  1. 1 2 3 4 5 6 7 8 9 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 5 6 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID   119257644.
  3. 1 2 Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
  4. 1 2 3 4 5 Ment, Kristo; et al. (2018). "Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810". The Astronomical Journal. 156 (5). 213. arXiv: 1809.01228 . Bibcode:2018AJ....156..213M. doi: 10.3847/1538-3881/aae1f5 . S2CID   119243619.
  5. 1 2 3 Gonzalez, G.; et al. (2010). "Parent stars of extrasolar planets - X. Lithium abundances and v sini revisited". Monthly Notices of the Royal Astronomical Society. 403 (3): 1368. arXiv: 0912.1621 . Bibcode:2010MNRAS.403.1368G. doi:10.1111/j.1365-2966.2009.16195.x. S2CID   118520284.
  6. ↑ "HD 86081". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2018-12-28.
  7. 1 2 "Approved names". NameExoworlds. Retrieved 2020-01-02.
  8. 1 2 3 Johnson, John Asher; et al. (2006). "The N2K Consortium. VI. Doppler Shifts without Templates and Three New Short-Period Planets". The Astrophysical Journal. 647 (1): 600–611. arXiv: astro-ph/0604348 . Bibcode:2006ApJ...647..600J. doi:10.1086/505173. S2CID   12421834.
  9. ↑ Pont, Frédéric (July 2009). "Empirical evidence for tidal spin-up in transiting planetary systems". Monthly Notices of the Royal Astronomical Society. 396 (3): 1789–1796. arXiv: 0812.1463 . Bibcode:2009MNRAS.396.1789P. doi:10.1111/j.1365-2966.2009.14868.x. S2CID   10975188.
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