| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 03h 49m 13.7393s[1] |
| Declination | +70° 52′ 15.781″[1] |
| Apparent magnitude (V) | 5.391 ± 0.009[2] |
| Characteristics | |
| Spectral type | kA2hA6VmA7[3] |
| U−B color index | +0.12[4] |
| B−V color index | +0.09[4] |
| Astrometry | |
| Radial velocity (Rv) | 17 ± 0.9[5] km/s |
| Proper motion (μ) | RA: 21.451(45) mas/yr[1] Dec.: −62.431(55) mas/yr[1] |
| Parallax (π) | 8.7759 ± 0.0632 mas[1] |
| Distance | 372 ± 3 ly (113.9 ± 0.8 pc) |
| Absolute magnitude (MV) | +0.11 |
| Orbit[6] | |
| Primary | HD 23277 A |
| Companion | HD 23277 B |
| Period (P) | 15.5132 d |
| Semi-major axis (a) | 43.0229 AU |
| Eccentricity (e) | 0.2210 |
| Argument of periastron (ω) (secondary) | 287.41° |
| Argument of periastron (ω) (primary) | 107.41° |
| Semi-amplitude (K1) (primary) | 22.20 km/s |
| Semi-amplitude (K2) (secondary) | 24.69 km/s |
| Details | |
| A | |
| Mass | 2.38 ± 0.13[7] M☉ |
| Radius | 3.55+0.16 −0.24[7] R☉ |
| Luminosity | 59.7[8] L☉ |
| Surface gravity (log g) | 3.72 ± 0.08[7] cgs |
| Temperature | 8,317+194 −189[7] K |
| Rotational velocity (v sin i) | 25 ± 5[9] km/s |
| Age | 610[10] Myr |
| B | |
| Mass | 2.11[6] M☉ |
| Rotational velocity (v sin i) | 25 ± 5[9] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 23277 (HR 1138) is a spectroscopic binary[11] located in the northern circumpolar constellation Camelopardalis. With a combined apparent magnitude of 5.39,[2] it is faintly visible to the naked eye under ideal conditions. This star is located at a distance of 372 light years,[1] but is drifting away at a rate of 17 km/s.[5]
The primary has a classification of kA2hA6VmA7,[3] which indicates that it has the calcium K-line of an A2 star, but its hydrogen lines suggest a class of A6 V and metallic lines of an A7 star. At present it has 2.38 times the Sun's mass, and 3.55 times its radius.[7] It radiates at 59.7 times the luminosity of the Sun[8] from its photosphere at an effective temperature of 8,317 K,[7] which gives it a white hue. The companion has 2.11 times the Sun's mass,[6] which suggests it is an A-type main-sequence star like the primary. Both stars spin at a projected rotational velocity of 25 km/s, common for an Am star.[9]
References
[edit]- ^ a b c d e 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 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361.
- ^ 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 Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
- ^ a b Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Carnegie Institute Washington D.C. Publication: 0. Bibcode:1953GCRV..C......0W.
- ^ a b c Kraicheva, Z.; Popova, E.; Tutukov, A.; Yungelson, L. (July 1980). "Catalogue of physical parameters of spectroscopic binary stars". Bulletin d'Information du Centre de Donnees Stellaires. 19: 71. Bibcode:1980BICDS..19...71K. ISSN 1169-8837.
- ^ a b c d e f 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 McDonald, I.; Zijlstra, A. A.; Watson, R. A. (October 2017). "Fundamental parameters and infrared excesses of Tycho-Gaia stars". Monthly Notices of the Royal Astronomical Society. 471 (1): 770–791. arXiv:1706.02208. Bibcode:2017MNRAS.471..770M. doi:10.1093/mnras/stx1433. ISSN 0035-8711.
- ^ a b c Howe, K. S.; Clarke, C. J. (January 2009). "An analysis of v sin (i) correlations in early-type binaries". Monthly Notices of the Royal Astronomical Society. 392 (1): 448–454. Bibcode:2009MNRAS.392..448H. doi:10.1111/j.1365-2966.2008.14073.x. ISSN 0035-8711.
- ^ "Digital Demo Room - Stellar Structure and Evolution Simulator". rainman.astro.illinois.edu. Retrieved 30 December 2021.
- ^ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (September 2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424: 727–732. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. ISSN 0004-6361.
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