Astronomy:BH Crucis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Crux |
| Right ascension | 12h 16m 16.7898187344s[2] |
| Declination | −56° 17′ 09.627987388″[2] |
| Apparent magnitude (V) | 6.55 - 10.1[3] |
| Characteristics | |
| Evolutionary stage | AGB[4] |
| Spectral type | SC4.5/8-e - SC7/8-e[5] (C8,2 in 2011)[4] |
| Variable type | Mira[3] |
| Astrometry | |
| Proper motion (μ) | RA: −5.009±0.065[2] mas/yr Dec.: −4.141±0.053[2] mas/yr |
| Parallax (π) | 0.9952 ± 0.0529[2] mas |
| Distance | 3,300 ± 200 ly (1,000 ± 50 pc) |
| Absolute magnitude (MV) | −4.80[6] |
| Details | |
| Mass | 2.55[7] M☉ |
| Radius | 216[2] R☉ |
| Luminosity | 13,700[4] L☉ |
| Surface gravity (log g) | −0.02[7] cgs |
| Temperature | 3,000[4] K |
| Metallicity [Fe/H] | −0.14[7] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
BH Crucis, also known as Welch's Red Variable, is a star in the constellation Crux. A long period (Mira-type) variable, its apparent magnitude ranges from 6.6 to 9.8 over 530 days.[3] Hence at its brightest it is barely visible with the unaided eye in a rural sky.[9] A red giant, it had been classified ranging between spectral types SC4.5/8-e and SC7/8-e,[3] but appears to have evolved into a C-type (carbon star) spectrum by 2011.[4]
Ronald G. Welch discovered the star while looking for new variables in October 1969. In the first thirty years since discovery, it has become redder and brighter (mean magnitude changing from 8.047 to 7.762) and its period lengthened by 25% from 421 to 530 days.[10] Retrospective examination of photographic plates taken in South West Africa in 1937 and 1951 and stored at Sonneberg Observatory suggest the amplitude of variation might have been smaller in the earliest records.[11] A study of the star published in 2011 found that the increase in period appeared to have stopped or even begun reversing (estimated at 524 days in 2011), and that the spectral class had changed from SC to C, with carbon emission becoming more prominent. Technetium was also recorded in the emission spectrum and its surface temperature deemed to have cooled to 3000 K.[4] Unusually for a Mira variable, BH Crucis had a double maximum, with two peaks in brightness, reminiscent of an RV Tauri variable. However, with the lengthening of its period, this feature disappeared.[10]
Guandalini and Cristallo calculated the luminosity of Mira variables based on their periods. Using a period of 421 days, they calculated the absolute magnitude of BH Crucis to be -4.80.[6] Uttenthaler and colleagues calculated a bolometric magnitude of -5.59.[4] Gaia Data Release 2 gives a parallax of 0.9952 mas and a corresponding distance of around 1000 pc.[2]
References
- ↑ "Download Data". AAVSO. https://www.aavso.org/data-download.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 Otero, Sebastian (6 January 2011). "BH Crucis". AAVSO Website. American Association of Variable Star Observers. http://www.aavso.org/vsx/index.php?view=detail.top&oid=10854. Retrieved 23 June 2014.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 Uttenthaler, S.; van Stiphout, K.; Voet, K.; van Winckel, H.; van Eck, S.; Jorissen, A.; Kerschbaum, F.; Raskin, G. et al. (2011). "The evolutionary state of Miras with changing pulsation periods". Astronomy & Astrophysics 531: 11. doi:10.1051/0004-6361/201116463. A88. Bibcode: 2011A&A...531A..88U.
- ↑ Samus, N. N. et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1 61 (1): 80–88. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ 6.0 6.1 Guandalini, R.; Cristallo, S. (2013). "Luminosities of carbon-rich asymptotic giant branch stars in the Milky Way". Astronomy & Astrophysics 555: 7. doi:10.1051/0004-6361/201321225. A120. Bibcode: 2013A&A...555A.120G.
- ↑ 7.0 7.1 7.2 Anders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardevol, J.; Casamiquela, L.; Figueras, F.; Jimenez-Arranz, O. et al. (2022). "VizieR Online Data Catalog: StarHorse2, Gaia EDR3 photo-astrometric distances (Anders+, 2022)". Vizier Online Data Catalog. Bibcode: 2022yCat.1354....0A.
- ↑ "V* BH Cru". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+BH+Cru.
- ↑ Bortle, John E. (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Sky Publishing Corporation. http://www.skyandtelescope.com/resources/darksky/3304011.html?page=1&c=y. Retrieved 25 June 2014.
- ↑ 10.0 10.1 Walker, W.S.G. (2009). "BH Crucis : Period, Magnitude, and Color Changes". J. Am. Assoc. Variable Star Obs. 37 (2): 87–95. Bibcode: 2009JAVSO..37...87W.
- ↑ Walker, W.S.G.; Marino, Brian F. (1972). "Welch's red variable star in Crux an R Centauri like variable". IAU Inform. Bull. Var. Stars 679: 1. Bibcode: 1972IBVS..679....1W.
 |  |
