Beta Caeli
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Caelum |
| Right ascension | 04h 42m 03.48029s[1] |
| Declination | −37° 08′ 39.4641″[1] |
| Apparent magnitude (V) | 5.04[2] |
| Characteristics | |
| Spectral type | F3 V[3] or F3 IV[4] |
| U−B color index | +0.01[2] |
| B−V color index | +0.38[2] |
| Astrometry | |
| Radial velocity (Rv) | 28.8±0.8[4] km/s |
| Proper motion (μ) | RA: +46.59[1] mas/yr Dec.: +193.56[1] mas/yr |
| Parallax (π) | 34.88 ± 0.42 mas[1] |
| Distance | 94 ± 1 ly (28.7 ± 0.3 pc) |
| Absolute magnitude (MV) | +2.64[5] |
| Details | |
| β Cae A | |
| Mass | 1.32[6] M☉ |
| Radius | 1.3[7] R☉ |
| Surface gravity (log g) | 4.09[6] cgs |
| Temperature | 6,763±230[6] K |
| Metallicity [Fe/H] | −0.12[3] dex |
| Rotational velocity (v sin i) | 97.5±4.9[5] km/s |
| Age | 1.753[6] Gyr |
| β Cae B | |
| Mass | 0.19[8] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
Beta Caeli (β Caeli, abbreviated to β Cae) is the Bayer designation for a star in the southern constellation of Caelum. It is a dim star but visible to the naked eye, having an apparent visual magnitude of 5.04.[2] Based upon an annual parallax shift of 4.88 mas as seen from Earth,[1] it is located 94 light years from the Sun. The star is moving away from the Sun with a radial velocity of +28.8 km/s.[4]
This is a probable single-lined spectroscopic binary star system.[10] The visible component has a stellar classification of F3 V[3] or F3 IV,[4] indicating it is either an F-type main-sequence star or a somewhat more evolved subgiant star, respectively. It has an estimated 1.3[6] times the mass of the Sun and about 1.3[7] times the Sun's radius. The star is 1.75[6] billion years old and has a high rate of spin with a projected rotational velocity of around 97.5 km/s.[5]
The companion is likely to be a low-mass (~0.2 M☉) star orbiting about 5 AU from the primary.[11] This object may be the source of the X-ray emission coming from the same location.[10]
References
[edit]- ^ a b c d e f van 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.
- ^ a b c d Cousins, A. W. J. (1973), "UBV photometry of some southern stars", Monthly Notes of the Astronomical Society of Southern Africa, 32: 11, Bibcode:1973MNSSA..32...11C.
- ^ a b c Gray, 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.
- ^ a b c d Torres, C. A. O.; et al. (December 2006), "Search for associations containing young stars (SACY). I. Sample and searching method", Astronomy and Astrophysics, 460 (3): 695–708, arXiv:astro-ph/0609258, Bibcode:2006A&A...460..695T, doi:10.1051/0004-6361:20065602, S2CID 16080025.
- ^ a b c Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
- ^ a b c d e f 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.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ García, Luciano H.; Petrucci, R.; Jofré, E.; Gómez, M. (2022). "High-contrast imaging of HD 29992 and HD 196385 with the Gemini Planet Imager". Monthly Notices of the Royal Astronomical Society. 515 (4): 4999–5008. doi:10.1093/mnras/stac1929.
- ^ "bet Cae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-09.
{{cite web}}: CS1 maint: postscript (link) - ^ a b Borgniet, Simon; et al. (2017), "Extrasolar planets and brown dwarfs around AF-type stars. IX. The HARPS southern sample", Astronomy & Astrophysics, 599: A57, arXiv:1608.08257, Bibcode:2017A&A...599A..57B, doi:10.1051/0004-6361/201628805, S2CID 118723455.
- ^ García, Luciano H.; Petrucci, R.; Jofré, E.; Gómez, M. (2022), High-contrast imaging of HD 29992 and HD 196385 with GPI, arXiv:2207.07435
