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

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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<span class="mw-page-title-main">HD 80606 and HD 80607</span> Binary star system in the constellation Ursa Major

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HD 45652 is a star with an exoplanetary companion in the equatorial constellation of Monoceros. It was officially named Lusitânia on 17 December 2019, after the IAU100 press conference in Paris by the IAU. This star has an apparent visual magnitude of 8.10, making it an 8th magnitude star that is too dim to be visible to the naked eye. The system is located at a distance of 114 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.188 arcsec yr−1.

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HD 175167 is a star with an exoplanet companion in the southern constellation of Pavo. It is too faint to be visible with the naked eye at an apparent visual magnitude of 8.01. The system is located at a distance of 232 light-years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.190 arcsec yr−1.

HD 38283, or Bubup, is a star in the southern circumpolar constellation Mensa. With an magnitude of 6.70, its invisible to the naked eye but can be seen with binoculars. Bubup is located relatively close at a distance of 124 light-years but is recceding with a heliocentric radial velocity of 61.4 km/s.

HD 7199 is a star in the constellation Tucana located 118 light years distance from the Sun based on parallax. It has an orange hue but is too dim to be viewed with the naked eye, having an apparent visual magnitude of +8.06. The star is drifting further away from the Sun with a radial velocity of +5.6 km/s.

HD 1690 is a giant star with an orbiting exoplanet companion in the constellation of Cetus. It has an apparent visual magnitude of 9.19, which is too faint to be visible to the naked eye. The distance to this system is approximately 2,570 light years, and it is drifting further away with a radial velocity of +18.2 km/s. HD 1690 has no known companion star, making it a single star system.

HD 22781, is a single star about 106 light-years away. It is a K-type main-sequence star. The star’s age is poorly constrained at 4.14±3.63 billion years, but is likely similar to that of the Sun. HD 22781 is heavily depleted in heavy elements, having just 45% of Sun's concentration of iron, yet is comparatively rich in carbon, having 90% of Sun`s abundance.

HD 121056, or HIP 67851, is an aging giant star with a pair of orbiting exoplanets located in the southern constellation of Centaurus. This star is dimly visible to the naked eye with an apparent visual magnitude of 6.17. It is located at a distance of 209 light years from the Sun, based on parallax measurements, and is drifting further away with a radial velocity of 5.6 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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