Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Auriga |
Right ascension | 05h 54m 50.76694s[1] |
Declination | +55° 42′ 25.0802″[1] |
Apparent magnitude (V) | +5.00[2] |
Characteristics | |
Spectral type | A2 Va[3] |
U−B color index | +0.12[2] |
B−V color index | +0.05[2] |
Astrometry | |
Radial velocity (Rv) | −13.3±2.4[4] km/s |
Proper motion (μ) | RA: −7.049[1] mas/yr Dec.: +12.959[1] mas/yr |
Parallax (π) | 13.3702 ± 0.1670 mas[1] |
Distance | 244 ± 3 ly (74.8 ± 0.9 pc) |
Absolute magnitude (MV) | +0.64[5] |
Details[6] | |
Mass | 1.96 M☉ |
Radius | 1.1[7] R☉ |
Luminosity | 49.5[5] L☉ |
Surface gravity (log g) | 3.88 cgs |
Temperature | 9,152±311 K |
Metallicity [Fe/H] | −0.36±0.04[5] dex |
Rotational velocity (v sin i) | 62 km/s |
Age | 174 Myr |
Other designations | |
Database references | |
SIMBAD | data |
Xi Aurigae, Latinized from ξ Aurigae, is the Bayer designation for a single,[9] white-hued star in the northern constellation of Auriga. This star was once considered part of the constellation of Camelopardalis and held the Flamsteed designation 32 Camelopardalis.[10] It is visible to the naked eye with an apparent visual magnitude of +5.0.[2] The measured annual parallax shift of this star is 13.37 ± 0.17 mas,[1] which corresponds to a physical distance of 244 light-years (75 parsecs) with a 3 light-year margin of error. At that distance, the visual magnitude of the star is diminished by an extinction of 0.108 due to interstellar dust.[11]
This is an A-type main sequence star with a stellar classification of A2 Va.[3] Although it was one of the first stars to be cataloged as a Lambda Boötis star, Murphy et al. (2015) don't consider it to be a member of this population.[3] The star has nearly twice[6] the mass of the Sun and about 1.1[7] times the Sun's radius. It is an estimated 174[6] million years old and is spinning with a projected rotational velocity of 62 km/s.[6] Xi Aurigae is radiating 49.5[5] times the Sun's luminosity from its photosphere at an effective temperature of around 9,152 K.[6]
References
[edit]- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
- ^ a b c Murphy, Simon J.; et al. (October 2015), "An Evaluation of the Membership Probability of 212 λ Boo Stars. I. A Catalogue", Publications of the Astronomical Society of Australia, 32: 43, arXiv:1508.03633, Bibcode:2015PASA...32...36M, doi:10.1017/pasa.2015.34, S2CID 59405545, e036.
- ^ de 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.
- ^ a b c d 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.
- ^ a b c d e David, 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.
- ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (Third ed.): 5211–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ "ksi Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-28.
- ^ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
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: CS1 maint: unflagged free DOI (link) - ^ Wagman, M. (August 1987), "Flamsteed's Missing Stars", Journal for the History of Astronomy, 18 (3): 213, Bibcode:1987JHA....18..209W, doi:10.1177/002182868701800305, S2CID 118445625.
- ^ Murphy, Simon J.; Paunzen, Ernst (April 2017), "Gaia's view of the λ Boo star puzzle", Monthly Notices of the Royal Astronomical Society, 466 (1): 546–555, arXiv:1612.01528, Bibcode:2017MNRAS.466..546M, doi:10.1093/mnras/stw3141, S2CID 119328659.
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: CS1 maint: unflagged free DOI (link)
Well, that’s interesting to know that Psilotum nudum are known as whisk ferns. Psilotum nudum is the commoner species of the two. While the P. flaccidum is a rare species and is found in the tropical islands. Both the species are usually epiphytic in habit and grow upon tree ferns. These species may also be terrestrial and grow in humus or in the crevices of the rocks.
View the detailed Guide of Psilotum nudum: Detailed Study Of Psilotum Nudum (Whisk Fern), Classification, Anatomy, Reproduction