DY Centauri
DY Centauri
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
Constellation | Centaurus |
Right ascension | 13h 25m 34.08s[1] |
Declination | −54° 14′ 43.1″[1] |
Apparent magnitude (V) | 13.2[2] |
| Characteristics | |
Spectral type | C-Hd/B5-6Ie[3] |
Variable type | RCB (inactive)[4] |
| Astrometry | |
| Radial velocity (Rv) | 21.30 ± 0.45[5] km/s |
| Distance | 23000 ly (7000[6] pc) |
| Absolute magnitude (MV) | -3[6] |
Orbit[5] | |
| Period (P) | 39.66779 ± 0.0088 days |
| Eccentricity (e) | 0.44 ± 0.10 |
| Periastron epoch (T) | 2445104.3364 ± 1.715 |
Argument of periastron (ω) (secondary) | 344.5 ± 16.7° |
Semi-amplitude (K1) (primary) | 13.26 ± 1.18 km/s |
| Details | |
| Mass | 0.8[5] M☉ |
| Radius | 8[5] R☉ |
| Surface gravity (log g) | 2.50 ± 0.12[2] cgs |
| Temperature | 24800 ± 600[2] K |
| Rotational velocity (v sin i) | 40 ± 5[2] km/s |
| Other designations | |
DY Centauri, 2MASS J13253407-5414431, AAVSO 1319–53[7] | |
| Database references | |
| SIMBAD | data |
DY Centauri is a variable star in the constellation Centaurus. From its brightness, it is estimated to be 7000 parsecs (23000 light-years) away from Earth.[6]
DY Centauri is classified as a R Coronae Borealis variable (RCB), a rare class of supergiant stars which show rapid and irregular decreases in brightness due to the formation of dust clouds on the stellar surface. However, DY Centauri is not an active RCB star anymore, and the last registered obscuration event was in 1934. This seems to be related to evolutionary changes in the star, represented by a very fast horizontal movement across the top of the HR diagram. Spectroscopic and photometric evidence show DY Centuari has increased its effective temperature from 5800 K in 1906 to 24800 K in 2010, while maintaining constant luminosity.[4] As consequence, its visual apparent magnitude has faded from about 11.75 in the beginning of the 20th century to 13.2 in 2010 (due to changes in the bolometric correction),[2] while its radius is calculated to have decreased from 100 R☉ to 8 R☉.[5] There are only three other known stars with this behavior, called hot RCB stars.[4]
Periodic changes in the radial velocity of DY Centauri have been detected, indicating that the star in a single-lined spectroscopic binary in an eccentric orbit (e = 0.44) with a period of 39.67 days. The companion star has an estimated minimum mass of 0.2 M☉, so it can be a low mass white dwarf or main sequence star. With an estimated separation of only 10 R☉ at periastron, the system must have interacted in the past when the primary had larger dimensions, forming a common envelope.[5]
DY Centauri has a peculiar chemical composition and is poor in hydrogen and rich in helium and carbon, being identified as an extreme helium star (EHe). In comparison to other RCB and EHe stars, however, its hydrogen content is relatively high.[2][8] Stars of this type are believed to be the product of the merger of two white dwarfs, therefore being single stars, which is inconsistent with the identification of DY Centauri as a close binary. Thus, the origin and evolutionary state of the DY Centauri system remain uncertain.[2] In the future, it is likely that the primary will evolve to a B subdwarf, a class of stars frequently found in binary systems.[5]
The spectrum of DY Centauri indicates the presence of a low density expanding nebula around it, formed by gas ionized by ultraviolet radiation from the star.[9] The nebula has an estimated dimension of 1.2 arcseconds and, from its expansion velocity, was probably created about a thousand years ago.[6]
References[edit]
^ ab Cutri, R. M.; et al. (2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog. 2246. Bibcode:2003yCat.2246....0C..mw-parser-output cite.citation{font-style:inherit}.mw-parser-output q{quotes:"""""""'""'"}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-limited a,.mw-parser-output .cs1-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png")no-repeat;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}
^ abcdefg Pandey, Gajendra; Kameswara Rao, N.; Jeffery, C. Simon; Lambert, David L. (October 2014). "On the Binary Helium Star DY Centauri: Chemical Composition and Evolutionary State". The Astrophysical Journal. 793 (2): article 76, 17 pp. arXiv:1408.3798. Bibcode:2014ApJ...793...76P. doi:10.1088/0004-637X/793/2/76.
^ Skiff, B. A (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009–2016)". VizieR On-line Data Catalog: B/mk. Originally published in: Lowell Observatory (October 2014). 1. Bibcode:2014yCat....1.2023S.
^ abc Schaefer, Bradley E. (August 2016). "All known hot RCB stars are fading fast over the last century". Monthly Notices of the Royal Astronomical Society. 460 (2): 1233–1242. arXiv:1605.02091. Bibcode:2016MNRAS.460.1233S. doi:10.1093/mnras/stw1065.
^ abcdefg Rao, N. Kameswara; et al. (November 2012). "The Hot R Coronae Borealis Star DY Centauri is a Binary". The Astrophysical Journal Letters. 760 (1): article L3, 6 pp. arXiv:1210.4199. Bibcode:2012ApJ...760L...3R. doi:10.1088/2041-8205/760/1/L3.
^ abcd Rao, N. Kameswara; Lambert, David L.; García-Hernández, D. A.; Manchado, Arturo (May 2013). "The changing nebula around the hot R Coronae Borealis star DY Centauri". Monthly Notices of the Royal Astronomical Society. 431 (1): 159–166. arXiv:1301.5773. Bibcode:2013MNRAS.431..159R. doi:10.1093/mnras/stt154.
^ "DY+Centauri". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-11-09.
^ Jeffery, C. S.; Heber, U. (March 1993). "Spectral analysis of DY Centauri, a hot R Coronae Borealis star with unusually high hydrogen content". Astronomy and Astrophysics. 270 (1–2): 167–176. Bibcode:1993A&A...270..167J.
^ Rao, N. Kameswara; Giridhar, S.; Lambert, D. L. (December 1993). "The hot R Coronae Borealis star DY Centauri: Nebular and photospheric lines". Astronomy and Astrophysics. 280 (1): 201–207. Bibcode:1993A&A...280..201R.
Categories:
- Centaurus (constellation)
- Objects with variable star designations
- R Coronae Borealis variables
- Spectroscopic binaries
- 2MASS objects
- B-type supergiants
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