HD 85390

Last updated
HD 85390 / Natasha
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Vela
Right ascension 09h 50m 02.4969s [1]
Declination –49° 47′ 24.9576″ [1]
Apparent magnitude  (V)8.54 [2]
Characteristics
Spectral type K1.5V [3]
Apparent magnitude  (B)9.395 [2]
Apparent magnitude  (J)7.012±0.024 [2]
Apparent magnitude  (H)6.612±0.033 [2]
Apparent magnitude  (K)6.491±0.023 [2]
B−V color index 0.855±0.003 [2]
Astrometry
Radial velocity (Rv)33.03±0.20 [4]  km/s
Proper motion (μ)RA: 29.8018±0.0379  mas/yr [1]
Dec.: −60.245±0.058  mas/yr [1]
Parallax (π)29.8018 ± 0.0379  mas [1]
Distance 109.4 ± 0.1  ly
(33.56 ± 0.04  pc)
Absolute magnitude  (MV)5.99 [2]
Details
Mass 0.81±0.02 M☉ [5]
0.813+0.043
−0.038 [6]   M☉
Radius 0.78±0.01 R☉ [5]
0.816+0.010
−0.011 [6]   R☉
Luminosity 0.39±0.01 [5]   L☉
Surface gravity (log g)4.56±0.02 [5]   cgs
Temperature 5,170±17 K [5]
5,182±20 [6]   K
Metallicity [Fe/H]–0.04 [6]   dex
Rotational velocity (v sin i)1.97±0.36 [6]  km/s
Age 6.8±2.9 Gyr [5]
8.893+4.400
−4.017 [6]   Gyr
Other designations
Natasha, CD–49°4727, Gaia DR2  5406324138654973824, HD  85390, HIP  48235, SAO  221526, 2MASS J09500249-4947250 [7]
Database references
SIMBAD data
Exoplanet Archive data
Extrasolar Planets
Encyclopaedia 		data

HD 85390 is a star with an exoplanet companion in the southern constellation of Vela. It was given the proper name Natasha by Zambia during the 100th anniversary of the IAU. Natasha means "thank you" in many languages of Zambia. [8] [9] This star is too faint to be seen with the naked eye, having an apparent visual magnitude of 8.54. [2] It is located at a distance of 109  light years from the Sun based on parallax, and is drifting further away with a radial velocity of 33 km/s. [1]

The stellar classification of HD 85390 is K1.5V, [3] showing this to be a K-type main-sequence star. It is an older star with age estimates of 7–9 billion years, and is not considered chromospherically active. [10] The star is spinning with a projected rotational velocity of 2 km/s. [6] It is smaller, cooler, dimmer, and less massive than the Sun, [5] but the metallicity is near solar. [6]

Planetary system

The planet b was detected by the radial velocity method in 2011. [10] It is following an eccentric orbit at a distance of 1.4  AU from the host star. [11] An additional planet in the system was suspected since 2013, [12] only to be refuted in 2019. [11]

The HD 85390 planetary system [11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b (Madalitso) ≥0.099 ± 0.010  MJ 1.373 ± 0.035799.52 ± 2.410.50 ± 0.05——

Related Research Articles

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HD 52265 is a 6th-magnitude G-type main sequence star located approximately 98 light-years away in the constellation of Monoceros. It is 21% more massive than and more than twice as luminous as the Sun. The age of the star is roughly 2.6 billion years. The star HD 52265 is named Citalá. The name was selected in the NameExoWorlds campaign by El Salvador, during the 100th anniversary of the IAU. Citalá means River of stars in the native Nahuat language.

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HR 7703 is a binary star system in the constellation of Sagittarius. The brighter component has an apparent visual magnitude of 5.31, which means it is visible from suburban skies at night. The two stars are separated by an angle of 7.10″, which corresponds to an estimated semimajor axis of 56.30 AU for their orbit.

HD 89744 is a star in the northern circumpolar constellation of Ursa Major, positioned about 0.4° due south of the bright star Tania Australis. This object has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.73. The distance to this star has been measured using the patallax method, which locates it 126 light years from the Sun. It is drifting closer with a radial velocity of −4.4 km/s. There are two known exoplanets orbiting this star.

HD 92788 is a star in the equatorial constellation of Sextans. It has a yellow hue but is too dim to be visible to the naked eye, having an apparent visual magnitude of 7.31. The star is located at a distance of 113 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −4.5 km/s. Two planets have been found in orbit around the star.

HD 52265 b, formally named Cayahuanca, is a gas giant exoplanet located approximately 98 light-years away in the constellation of Monoceros, orbiting the star HD 52265. The planet has a minimum mass slightly more than that of Jupiter. Mean distance between the planet and the star is half that of Earth from the Sun. It was discovered by both the California and Carnegie Planet Search team and the Geneva Extrasolar Planet Search team independently of each other. By studying the fluctuations of the brightness of a host star, the inclination of the stars equator was determined. This allowed to calculate its true mass, assuming that the planet orbits in the plane of the star's equator.

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<span class="mw-page-title-main">HD 114613</span> Star in the constellation Centaurus

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<span class="mw-page-title-main">HD 199223</span> Double star in the constellation Delphinus.

HD 199223 is a double star in the equatorial constellation Delphinus. However, the system was originally in Equuleus prior to the creation of official IAU constellation borders. The components have a separation of 2″ at a position angle of 282° as of 2016. They have apparent magnitudes of 6.34 and 7.49 and distances of 354 and 359 light years respectively. The system is drifting closer with a radial velocity of −33 km/s.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 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 Gray, R.O.; et al. (July 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.
  4. ↑ 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.
  5. 1 2 3 4 5 6 7 Bonfanti, A.; Ortolani, S.; Nascimbeni, V. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: 14. arXiv: 1511.01744 . Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID   53971692. A5.
  6. 1 2 3 4 5 6 7 8 Soto, M. G.; Jenkins, J. S. (2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy and Astrophysics. 615: A76. arXiv: 1801.09698 . Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. S2CID   119107228.
  7. ↑ "HD 85390". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-09-26.
  8. ↑ "Approved names". NameExoworlds. Retrieved 2020-01-02.
  9. ↑ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  10. 1 2 Mordasini, C.; et al. (2011). "The HARPS search for southern extrasolar planets XXIV. Companions to HD 85390, HD 90156, and HD 103197: a Neptune analog and two intermediate-mass planets". Astronomy and Astrophysics. 526. A111. arXiv: 1010.0856 . Bibcode: 2011A&A...526A.111M . doi: 10.1051/0004-6361/200913521 .
  11. 1 2 3 Wittenmyer, Robert A.; Clark, Jake T.; Zhao, Jinglin; Horner, Jonathan; Wang, Songhu; Johns, Daniel (2019), "Truly eccentric. I. Revisiting eight single-eccentric planetary systems", Monthly Notices of the Royal Astronomical Society, 484 (4): 5859–5867, arXiv: 1901.08471 , Bibcode:2019MNRAS.484.5859W, doi:10.1093/mnras/stz290, S2CID   118915974
  12. ↑ Wittenmyer, Robert A.; et al. (2013), "Forever alone? Testing single eccentric planetary systems for multiple companions", The Astrophysical Journal Supplement Series, 208 (1): 2, arXiv: 1307.0894 , Bibcode:2013ApJS..208....2W, doi:10.1088/0067-0049/208/1/2, S2CID   14109907
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