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C Hydrae

From Wikipedia, the free encyclopedia
Star in the constellation Hydra
C Hydrae
Location of C Hydrae (circled)
Observation data
Epoch J2000      Equinox J2000
ConstellationHydra[1]
Right ascension08h 25m 39.63201s[2]
Declination−03° 54′ 23.1178″[2]
Apparent magnitude (V)3.90[3]
Characteristics
Evolutionary stagemain sequence[4]
Spectral typeA0 Va[5]
B−Vcolor index−0.012±0.003[1]
Astrometry
Radial velocity (Rv)+10.00±1.78[6] km/s
Proper motion (μ)RA: −66.43[2]mas/yr
Dec.: −23.41[2]mas/yr
Parallax (π)26.66±0.19 mas[2]
Distance122.3 ± 0.9 ly
(37.5 ± 0.3 pc)
Absolute magnitude (MV)1.04[1]
Details
Mass2.3[7] M
Radius2.5[7] R
Luminosity37[7] L
Surface gravity (log g)4.20[8] cgs
Temperature9,074[7] K
Metallicity[Fe/H]−0.04[9] dex
Rotational velocity (v sin i)129[8] km/s
Age162[8] Myr
Other designations
C Hya,30 Mon,BD−03°2339,HD 71155,HIP 41307,HR 3314,SAO 135896[10]
Database references
SIMBADdata

C Hydrae is a single[11]star in theequatorialconstellation ofHydra,[10] located 122 light years away from the Sun.[2] It has theFlamsteed designation30 Monocerotis,[10] assigned when it belonged to the constellationMonoceros. The object is visible to the naked eye as a white-hued star with anapparent visual magnitude of 3.90.[3] It is moving away from the Earth with a heliocentricradial velocity of +10 km/s.[6]

This is anA-type main-sequence star with astellar classification of A0 Va.[5] It is around 162[8] million years old with a high rate of spin, showing aprojected rotational velocity of 129 km/s. The star has 2.3 times themass of the Sun and about 2.5 times theSun's radius. It is radiating 37 times theluminosity of the Sun from itsphotosphere at aneffective temperature of 9,074 K.

Astatistically significantinfrared excess has been detected, indicating adebris disk is orbiting2.0±0.1 AU from the host star with ablackbody temperature of499±3 K. It is comparable in size to theasteroid belt.[12] UnexplainedX-ray emission has also been detected coming from these coordinates – stars of this class are not normally expected to show X-ray emission, so it may be coming from a background source or an unseen companion.[13]

References

[edit]
  1. ^abcAnderson, 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. XHIP record for this object atVizieR.
  2. ^abcdefvan Leeuwen, F. (2007), "Validation of the new Hipparcos reduction",Astronomy and Astrophysics,474 (2):653–664,arXiv:0708.1752,Bibcode:2007A&A...474..653V,doi:10.1051/0004-6361:20078357,S2CID 18759600.
  3. ^abBaines, Ellyn K.; et al. (2018), "Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer",The Astronomical Journal,155 (1), 30,arXiv:1712.08109,Bibcode:2018AJ....155...30B,doi:10.3847/1538-3881/aa9d8b,S2CID 119427037.
  4. ^Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities".Astronomy and Astrophysics.537: A120.arXiv:1201.2052.Bibcode:2012A&A...537A.120Z.doi:10.1051/0004-6361/201117691.
  5. ^abGray, 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.
  6. ^abde Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project",Astronomy & Astrophysics,546: 14,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID 59451347, A61.
  7. ^abcdHardegree-Ullman, Kevin K.; Apai, Dániel; Bergsten, Galen J.; Pascucci, Ilaria; López-Morales, Mercedes (2023), "Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O2 Levels in Nearby Transiting Habitable-zone Exoplanets",The Astronomical Journal,165 (6): 267,arXiv:2304.12490,Bibcode:2023AJ....165..267H,doi:10.3847/1538-3881/acd1ec.
  8. ^abcdDavid, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets",The Astrophysical Journal,804 (2): 146,arXiv:1501.03154,Bibcode:2015ApJ...804..146D,doi:10.1088/0004-637X/804/2/146,S2CID 33401607.
  9. ^Gáspár, András; Rieke, George H.; Ballering, Nicholas (2016), "The Correlation between Metallicity and Debris Disk Mass",The Astrophysical Journal,826 (2): 171,arXiv:1604.07403,Bibcode:2016ApJ...826..171G,doi:10.3847/0004-637X/826/2/171.
  10. ^abc"30 Mon",SIMBAD,Centre de données astronomiques de Strasbourg, retrievedMay 7, 2019.
  11. ^Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems",Monthly Notices of the Royal Astronomical Society,389 (2):869–879,arXiv:0806.2878,Bibcode:2008MNRAS.389..869E,doi:10.1111/j.1365-2966.2008.13596.x,S2CID 14878976.
  12. ^Moerchen, Margaret M.; et al. (November 2010), "High Spatial Resolution Imaging of Thermal Emission from Debris Disks",The Astrophysical Journal,723 (2):1418–1435,arXiv:1011.1410,Bibcode:2010ApJ...723.1418M,doi:10.1088/0004-637X/723/2/1418,S2CID 118648798.
  13. ^Schröder, C.; Schmitt, J. H. M. M. (November 2007), "X-ray emission from A-type stars",Astronomy and Astrophysics,475 (2):677–684,Bibcode:2007A&A...475..677S,doi:10.1051/0004-6361:20077429.
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