| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 00h 35m 32.833s[1] |
| Declination | −00° 30′ 20.20″[1] |
| Apparent magnitude (V) | 5.84[2] |
| Characteristics | |
| Evolutionary stage | Hertzsprung gap[3] |
| Spectral type | F5 V[4][5] or F5 IV[2] |
| B−V color index | 0.444±0.006[6] |
| Astrometry | |
| Radial velocity (Rv) | +11.3±0.2[7] km/s |
| Proper motion (μ) | RA: +143.173 mas/yr[1] Dec.: −62.295 mas/yr[1] |
| Parallax (π) | 17.4181 ± 0.0314 mas[1] |
| Distance | 187.3 ± 0.3 ly (57.4 ± 0.1 pc) |
| Absolute magnitude (MV) | 2.26±0.04[8] |
| Details | |
| Mass | 1.55±0.1[2] M☉ |
| Radius | 2.6[2] R☉ |
| Luminosity | 10.7[2] L☉ |
| Surface gravity (log g) | 3.87±0.15[9] cgs |
| Temperature | 6,583±90[9] K |
| Metallicity [Fe/H] | −0.11±0.06[9] dex |
| Rotational velocity (v sin i) | 5[2] km/s |
| Age | 2.1±0.4[9] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
14 Ceti is a single[11] star in the equatorial constellation of Cetus. It is faintly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.84.[2] The distance to 14 Ceti can be estimated from its annual parallax shift of 17.4″,[1] which puts it 187 light years away. It is moving further from the Earth with a heliocentric radial velocity of +11 km/s,[7] having recently come no closer than 178 ly.[6]
Gray (1989) as well as Houk and Swift (1999) have this star classified as an F-type main-sequence star with a stellar classification of F5 V.[4][5] However, in the 5th revised edition of the Bright Star Catalogue it was classed by Hoffleit and Warren (1991) as a more evolved subgiant star with a class of F5 IV.[12] The absolute magnitude and effective temperature for this star shows that it is entering the Hertzsprung gap, which is occupied by a class of stars that have consumed the hydrogen at their core but have not yet begun hydrogen fusion along a shell surrounding the center.[11]
Evolutionary models for this star give an estimated age of around 2.1[9] billion years with 1.6[2] times the mass of the Sun. It has 2.6[2] times the Sun's radius and is radiating 10.7[2] times the Sun's luminosity from its photosphere at an effective temperature of about 6,583 K.[9] There is a thin convective envelope near its surface.[2] The star has a lower abundance of elements more massive than helium – what astronomers' term the metallicity – compared to the Sun.[9] The projected rotational velocity is a relatively low 5 km/s, but the rotation rate is unknown since the axial tilt hasn't been determined.[2]
14 Ceti shows an X-ray emission of 0.33×1030 erg s−1, which is on the high side for an F5 star. Both the corona and chromosphere of this star show indications of a magnetic field, and a surface field was detected in 2009 with a strength of −30 G. This made it the only known star between classes F0 and F7 to have a Zeeman effect detected. Two possible explanations for this field are that it is a fast rotator with a dynamo-driven field, or that it is a former Ap star.[11] The activity properties of this star make it more likely to be the latter.[3]
References[edit]
- ^ a b c d e 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.
- ^ a b c d e f g h i j k l Aurière, M.; et al. (February 2015), "The magnetic fields at the surface of active single G-K giants", Astronomy & Astrophysics, 574: 30, arXiv:1411.6230, Bibcode:2015A&A...574A..90A, doi:10.1051/0004-6361/201424579, S2CID 118504829, A90.
- ^ a b Aurière, M.; et al. (November 2014), "Descendants of magnetic and non-magnetic A-type stars", in Mathys, G.; Griffin, E.; Kochukhov, O.; Monier, R.; Wahlgren, G. (eds.), Putting A Stars into Context: Evolution, Environment, and Related Stars, Proceedings of the international conference held on June 3-7, 2013 at Moscow M.V. Lomonosov State University in Moscow, Russia, Moscow: Pero, pp. 444–450, arXiv:1310.6942, Bibcode:2014psce.conf..444A.
- ^ a b Gray, R. O. (1989), "The extension of the MK spectral classification system to the intermediate population II F type stars", Astronomical Journal, 98 (3): 1049–1062, Bibcode:1989AJ.....98.1049G, doi:10.1086/115195.
- ^ a b Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Ann Arbor, Michigan: Department of Astronomy, University of Michigan, Bibcode:1999MSS...C05....0H.
- ^ a b 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 Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
- ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
- ^ a b c d e f g Bensby, T.; et al. (2014), "Exploring the Milky Way stellar disk. A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood", Astronomy & Astrophysics, 562 (A71): 28, arXiv:1309.2631, Bibcode:2014A&A...562A..71B, doi:10.1051/0004-6361/201322631, S2CID 118786105.
- ^ "14 Cet". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved December 20, 2018.
- ^ a b c Aurière, M.; et al. (July 2012), "14 Ceti: a probable Ap-star-descendant entering the Hertzsprung gap", Astronomy & Astrophysics, 543: 6, arXiv:1205.6962, Bibcode:2012A&A...543A.118A, doi:10.1051/0004-6361/201219324, S2CID 118482901, A118.
- ^ Hoffleit, D.; Warren, W. H. Jr. (November 1995), "Bright Star Catalogue", VizieR Online Data Catalog (5th Revised ed.), Bibcode:1995yCat.5050....0H.
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