| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 10h 29m 41.6297s[1] |
| Declination | +84° 15′ 06.949″[1] |
| Apparent magnitude (V) | 5.51±0.01[2] |
| Characteristics | |
| Spectral type | A9 V[3] |
| U−B color index | +0.06[2] |
| B−V color index | +0.23[2] |
| Astrometry | |
| Radial velocity (Rv) | 3.5±2[4] km/s |
| Proper motion (μ) | RA: −145.145 mas/yr[1] Dec.: −21.494 mas/yr[1] |
| Parallax (π) | 23.0490 ± 0.3729 mas[1] |
| Distance | 142 ± 2 ly (43.4 ± 0.7 pc) |
| Absolute magnitude (MV) | +2.48[5] |
| Orbit[6] | |
| Primary | A |
| Companion | B |
| Period (P) | 2.20±0.03 yr |
| Semi-major axis (a) | 0.0142±0.0006″ |
| Eccentricity (e) | 0.26±0.11 |
| Details | |
| A | |
| Mass | 1.69[7] M☉ |
| Radius | 1.79[1] R☉ |
| Luminosity | 8.4[8] L☉ |
| Surface gravity (log g) | 4.27[9] cgs |
| Temperature | 7,535[10] K |
| Metallicity [Fe/H] | +0.04[11] dex |
| Rotational velocity (v sin i) | 134±7[10] km/s |
| Age | 710[7] Myr |
| B | |
| Mass | 0.38[7] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 89571 (HR 4062) is a binary star[12] located in the northern circumpolar constellation Camelopardalis. It is faintly visible to the naked eye with a combined apparent magnitude of 5.51[2] and is estimated to be 142 light years[1] away from the Solar System. However, it is receding with a heliocentric radial velocity of 3.5 km/s.[4]
The primary has a stellar classification of A9 V,[3] indicating that it is an ordinary A-type main-sequence star. David S. Evans gave it a slightly warmer class of A6 V[13] while Cowley et al. classified it as F0 IV,[14] indicating a F-type subgiant. Nevertheless, the two components take roughly 2 years to orbit each other at a mean separation of 14.2 mas.[6]
The components have masses of 1.69 M☉ and 0.38 M☉,[7] with the latter being a probable M-type star. HD 89571 has a radius of 1.79 R☉[1] and a luminosity of 8.4 L☉.[8] This yields an effective temperature of 7,535 K,[10] giving a white hue. It is estimated to be 710 million years old[7] and spins rapidly with a projected rotational velocity of 134 km/s;[10] it has a near solar metallicity, equating to an iron abundance 110% that of the Sun.[11]
References
[edit]- ^ a b c d e f g 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.
- ^ a b c d Oja, T. (August 1991). "UBV photometry of stars whose positions are accurately known. VI". Astronomy and Astrophysics Supplement Series. 89: 415. Bibcode:1991A&AS...89..415O. ISSN 0365-0138.
- ^ a b Abt, Helmut A.; Morrell, Nidia I. (July 1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182. ISSN 0067-0049.
- ^ a b Evans, D. S. (1967). "The Revision of the General Catalogue of Radial Velocities". International Astronomical Union. 30: 57. Bibcode:1967IAUS...30...57E.
- ^ 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 Malkov, O. Yu.; Tamazian, V. S.; Docobo, J. A.; Chulkov, D. A. (October 2012). "Dynamical masses of a selected sample of orbital binaries". Astronomy & Astrophysics. 546: A69. Bibcode:2012A&A...546A..69M. doi:10.1051/0004-6361/201219774. eISSN 1432-0746. ISSN 0004-6361.
- ^ a b c d e De Rosa, R. J.; Patience, J.; Wilson, P. A.; Schneider, A.; Wiktorowicz, S. J.; Vigan, A.; Marois, C.; Song, I.; Macintosh, B.; Graham, J. R.; Doyon, R.; Bessell, M. S.; Thomas, S.; Lai, O. (26 November 2013). "The VAST Survey – III. The multiplicity of A-type stars within 75 pc". Monthly Notices of the Royal Astronomical Society. 437 (2): 1216–1240. arXiv:1311.7141. Bibcode:2014MNRAS.437.1216D. doi:10.1093/mnras/stt1932. eISSN 1365-2966. ISSN 0035-8711.
- ^ a b Chandler, Colin Orion; McDonald, Iain; Kane, Stephen R. (17 February 2016). "The Catalog of Earth-Like Exoplanet Survey Targets (CELESTA): A Database of Habitable Zones Around Nearby Stars". The Astronomical Journal. 151 (3): 59. arXiv:1510.05666. Bibcode:2016AJ....151...59C. doi:10.3847/0004-6256/151/3/59. eISSN 1538-3881.
- ^ Allende Prieto, C.; Lambert, D. L. (December 1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: masses, radii and effective temperatures". Astronomy and Astrophysics. 352: 555–562. arXiv:astro-ph/9911002. Bibcode:1999A&A...352..555A. ISSN 0004-6361.
- ^ a b c d Reiners, A. (January 2006). "Rotation- and temperature-dependence of stellar latitudinal differential rotation". Astronomy & Astrophysics. 446 (1): 267–277. arXiv:astro-ph/0509399. Bibcode:2006A&A...446..267R. doi:10.1051/0004-6361:20053911. eISSN 1432-0746. ISSN 0004-6361.
- ^ a b Netopil, Martin (4 May 2017). "Metallicity calibrations for dwarf stars and giants in the Geneva photometric system". Monthly Notices of the Royal Astronomical Society. 469 (3): 3042–3055. arXiv:1705.00883. Bibcode:2017MNRAS.469.3042N. doi:10.1093/mnras/stx1077. eISSN 1365-2966. ISSN 0035-8711.
- ^ Eggleton, P. P.; Tokovinin, A. A. (11 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. eISSN 1365-2966. ISSN 0035-8711.
- ^ Evans, D. S. (1966). "Fundamental data for Southern stars (6th list)". Royal Greenwich Observatory Bulletins. 110: 185. Bibcode:1966RGOB..110..185E.
- ^ Cowley, A.; Cowley, C.; Jaschek, M.; Jaschek, C. (April 1969). "A study of the bright stars. I. A catalogue of spectral classifications". The Astronomical Journal. 74: 375. Bibcode:1969AJ.....74..375C. doi:10.1086/110819. ISSN 0004-6256.
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