HD 203030

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HD 203030
Spitzer IRAC HD 203030B.jpg
HD 203030 and its companion (white arrow) with Spitzer IRAC.
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Vulpecula
Right ascension 21h 18m 58.220s [1]
Declination 26° 13′ 49.96″ [1]
Apparent magnitude  (V)8.45 [2]
Characteristics
Evolutionary stage main sequence
Spectral type K0V [3]
B−V color index 0.750±0.015 [2]
Variable type BY Dra [4]
Astrometry
Radial velocity (Rv)−16.92±0.26 [5]  km/s
Proper motion (μ)RA: 133.593±0.108  mas/yr [1]
Dec.: 9.563±0.11  mas/yr [1]
Parallax (π)25.4488 ± 0.0610  mas [1]
Distance 128.2 ± 0.3  ly
(39.29 ± 0.09  pc)
Absolute magnitude  (MV)5.436±0.030 [6]
Details
Mass 0.965±0.035 [7]   M☉
Radius 0.86+0.02
−0.03 [5]   R☉
Luminosity 0.593±0.002 [5]   L☉
Surface gravity (log g)4.64+0.03
−0.01 [8]   cgs
Temperature 5,603+10
−8 [8]   K
Metallicity [Fe/H]0.06±0.07 dex
0.30+0.02
−0.01 [8]   dex
Rotational velocity (v sin i)5.62+0.13
−0.14 [8]  km/s
Age 100+50
−70 [9]   Myr
Other designations
V457 Vul, Gaia DR2  1846882224145757056, HD  203030, HIP  105232, WDS 21190+2614, LTT  4041, TYC  2190-1095-1, 2MASS J21185820+2613500 [10]
Database references
SIMBAD data
Exoplanet Archive data

HD 203030, also known as V457 Vulpeculae, is a single, yellow-orange hued star with a sub-stellar companion in the northern constellation of Vulpecula. The designation HD 203030 is from the Henry Draper Catalogue , which is based on spectral classifications made between 1911 and 1915 by Annie Jump Cannon and her co-workers, and was published between 1918 and 1924. This star is invisible to the naked eye, having an apparent visual magnitude of 8.45. [2] It is located at a distance of 128  light years from the Sun based on parallax, [1] and is drifting closer with a radial velocity of −17 km/s. [5]

A light curve for V457 Vulpeculae, plotted from TESS data. The period listed in the GCVS is marked in red. V457VulLightCurve.png
A light curve for V457 Vulpeculae, plotted from TESS data. The period listed in the GCVS is marked in red.

The stellar classification of HD 203030 is K0V, [3] indicating this is a K-type main-sequence star. [3] It is likely very young, belonging to the 45 million years old IC 2391 open cluster. [9] Based on photometric measurements by Hipparcos, it was found to exhibit low amplitude periodic variability with a range of 0.0139 in magnitude and a period of 4.14 days. [12] However the General Catalog of Variable Stars lists its period as 6.664 days. [4] It is now classified as a chromospherically active BY Draconis variable. [4] The star has 97% [7] of the mass of the Sun and 86% [5] of the Sun's radius. It is radiating 59% [5] of the luminosity of the Sun from its photosphere at an effective temperature of 5,603 K. [8]

Planetary system

In 2006, direct imaging found co-moving companion at a projected separation of 487.1±1.8  AU , suggesting this is a candidate brown dwarf of spectral class L7.5. [13] It was shown to be in a bound orbit around the star by 2014. [7] In 2017, a reanalysis indicated that the star HD 203030 is probably very young, and therefore both the primary and the observed companion are less massive than previously thought. This places the companion object at the planetary mass boundary. [9] In 2019, the rotational period of HD 203030 B was measured as 7.5+0.6
−0.5 hours, and a patchy cloud cover was detected. [6]

The HD 203030 planetary system [9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
B11+4
−3  MJ 		487————

Related Research Articles

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HD 106252 is a star with a brown dwarf companion in the constellation Virgo. An apparent visual magnitude of 7.41 means this star is too faint to be visible to the naked eye. It is located at a distance of 210 light years from the Sun based on parallax measurements, and is receding with a radial velocity of 15 km/s.

HD 111232 is a star in the southern constellation of Musca. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 7.59. The distance to this star is 94.5 light years based on parallax. It is drifting away from the Sun with a radial velocity of +104 km/s, having come to within 14.1 light-years some 264,700 years ago. The absolute magnitude of this star is 5.25, indicating it would have been visible to the naked eye at that time.

HD 190228 is a star with an orbiting substellar companion in the northern constellation of Vulpecula. Its apparent magnitude is 7.30 – too faint to be seen with the naked eye – and the absolute magnitude is 3.34. Based on parallax measurements, it is located at a distance of 205 light-years from the Sun. The system is drifting closer with a radial velocity of −50 km/s.

HD 213240 is a possible binary star system in the constellation Grus. It has an apparent visual magnitude of 6.81, which lies below the limit of visibility for normal human sight. The system is located at a distance of 133.5 light years from the Sun based on parallax. The primary has an absolute magnitude of 3.77.

<span class="mw-page-title-main">HD 13189</span> Orange-hued star in the constellation Taurus

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HD 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s.

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 156279 is a star with a pair of orbiting exoplanets located in the northern constellation of Draco. It has various alternate designations, including HIP 84171 and BD+63 1335. Parallax measurements yield a distance of 118 light years from the Sun, but it is drifting closer with a radial velocity of −20 km/s. Despite an absolute magnitude of 5.25, at that distance the star is too faint to be visible to the naked eye with an apparent visual magnitude of 8.17. It is presumed to be a single star, as in 2019 all imaging surveys have failed to find any stellar companions.

HD 164509 is a binary star system in the constellation of Ophiuchus. The primary component has an orbiting exoplanet companion. This system is located at a distance of 175 light years based on parallax measurements, and is drifting further away with a radial velocity of 13.7 km/s. It has an absolute magnitude of 4.64, but at that distance the system has an apparent visual magnitude of 8.10, which is too faint to be seen with the naked eye.

HD 217786 is a binary star system in the equatorial constellation of Pisces. With an apparent visual magnitude of 7.78, it requires binoculars or a small telescope to view. The system is located at a distance of 181 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s. Kinematically, the star system belongs to the thin disk population of the Milky Way.

HD 7449 is a binary star system about 126 light-years way. The primary star, HD 7449 A, is a main-sequence star belonging to the spectral class F9.5. It is younger than the Sun. The primary star is slightly depleted of heavy elements, having 80% of solar abundance.

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HD 203473 is a star in the equatorial constellation Equuleus. With an apparent magnitude of 8.23, it’s only visible by using an amateur telescope. The star is located at a distance of 237 light years based on its parallax shift but is drifting closer at a high rate of 61.7 km/s. As of 2014, no stellar companions have been detected around the star.

HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.

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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 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 3 Frasca, A.; et al. (May 1, 2018). "A spectroscopic survey of the youngest field stars in the solar neighborhood . II. The optically faint sample". Astronomy and Astrophysics. 612: A96. arXiv: 1801.00671 . Bibcode:2018A&A...612A..96F. doi:10.1051/0004-6361/201732028. ISSN   0004-6361. S2CID   119537437.
  4. 1 2 3 Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID   255195566.
  5. 1 2 3 4 5 6 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.
  6. 1 2 Miles-Páez, Paulo A.; et al. (2019). "Cloud Atlas: Variability in and out of the Water Band in the Planetary-mass HD 203030B Points to Cloud Sedimentation in Low-gravity L Dwarfs". The Astrophysical Journal. 883 (2): 181. arXiv: 1908.09403 . Bibcode:2019ApJ...883..181M. doi: 10.3847/1538-4357/ab3d25 . S2CID   201696377.
  7. 1 2 3 Ginski, C.; et al. (2014). "Astrometric follow-up observations of directly imaged sub-stellar companions to young stars and brown dwarfs★". Monthly Notices of the Royal Astronomical Society. 444 (3): 2280–2302. arXiv: 1409.1850 . Bibcode:2014MNRAS.444.2280G. doi: 10.1093/mnras/stu1586 . S2CID   119118750.
  8. 1 2 3 4 5 Swastik, C.; et al. (March 2021). "Host Star Metallicity of Directly Imaged Wide-orbit Planets: Implications for Planet Formation". The Astronomical Journal. 161 (3): 13. arXiv: 2012.13694 . Bibcode:2021AJ....161..114S. doi: 10.3847/1538-3881/abd802 . S2CID   229679749. 114.
  9. 1 2 3 4 Miles-Páez, Paulo A.; et al. (2017). "The Prototypical Young L/T-Transition Dwarf HD 203030B Likely Has Planetary Mass". The Astronomical Journal. 154 (6): 262. arXiv: 1710.11274 . Bibcode:2017AJ....154..262M. doi: 10.3847/1538-3881/aa9711 . S2CID   67821107.
  10. ↑ "HD 203030". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2022-01-28.{{cite web}}: CS1 maint: postscript (link)
  11. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 27 May 2022.
  12. ↑ Koen, Chris; Eyer, Laurent (March 2002). "New periodic variables from the Hipparcos epoch photometry". Monthly Notices of the Royal Astronomical Society. 331 (1): 45–59. arXiv: astro-ph/0112194 . Bibcode:2002MNRAS.331...45K. doi: 10.1046/j.1365-8711.2002.05150.x . S2CID   10505995.
  13. ↑ Metchev, Stanimir A.; Hillenbrand, Lynne A. (2006). "HD 203030B: An Unusually Cool Young Substellar Companion near the L/T Transition". The Astrophysical Journal. 651 (2): 1166–1176. arXiv: astro-ph/0607514 . Bibcode:2006ApJ...651.1166M. doi:10.1086/507836. S2CID   16571973.
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