}}{{Starbox reference|Simbad=SX+Cen}}{{starbox end}}SX Centauri is a variable star in the constellation Centaurus. An RV Tauri variable, its light curve alternates between deep and shallow minima, varying its apparent magnitude from 9.1 to 12.4.[3] From the period-luminosity relationship, it is estimated to be around 1.6 kpc (5200 light-years) from Earth.[6] Gaia Data Release 2 gives a parallax of 0.2175 mas, corresponding to distance of about {{val|4,600|ul=pc|fmt=commas}}.[1]RV Tauri variables like SX Centauri are supergiant pulsating stars and a subtype of the population II Cepheids. They are stars that have already passed the asymptotic giant branch (AGB) and are in the last stage of their evolution before becoming a planetary nebula. This transition phase is very fast, and may last for less than a thousand years.[4] SX Centauri is in the beginning of this process and is estimated to be leaving the AGB right now, or to have left the AGB a few decades ago. Its pulsations are radial in nature and have a period of about 32.9 days (from deep minimum to deep minimum), causing the effective temperature of the star to vary between 5,000 and 6,500 K and the radius between 21 and 29 solar radii. The radius seems to have the same value in both the primary and secondary minima, while the temperature shows a 500 K variation between minima.[23]
The spectrum of SX Centauri shows infrared excess, indicating the presence of a circumstellar disk of hot dust around the star. interferometric observations constrained the diameter of the disk to less than 11 arcseconds (18 AU at the star's distance), indicating a very compact system.[6] The infrared emission is consistent with a hotter component (715 K) corresponding to 4% of the dust, and a colder one (244 K) correspoding to 96% of the dust. This material is composed mainly of amorphous carbon and graphite (83%), with the remainder being pyroxene and olivine.[4] The disk is related to a depletion of refractory elements (with high condensation temperature) in the star's photosphere; this is caused by separation of gas from dust rich in refractories, followed by accretion of the gas by the star.[5]
SX Centauri is a spectroscopic binary, having a companion star with an orbital period of 592 days and an orbital eccentricity of 0.16. This companion has a mass estimated between 1.4 and 1.9 solar masses and is probably an unevolved main sequence star. The system must have interacted in the past when the primary was a red giant, which is likely related to the formation of disk.[6] All RV Tauri stars with dust disks are believed to be part of a binary system.[28]
Slow periodic variations in the mean brightness of SX Centauri have been detected, leading the star to be classified as an RV Tauri star of the photometric class b (RVb). The period of this variation is approximately equal to the orbital period of the system. This phenomenon can be explained as variation of the circumstellar extinction during the orbital motion of the disk.[5]
References
1. ^1 2 {{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S|volume=1|display-authors=etal|author1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}
2. ^1 2 3 4 5 6 {{cite DR2|6127031608094036864}}
3. ^1 {{cite journal|author=Manick, Rajeev |author2=Van Winckel, Hans |author3=Kamath, Devika |author4=Hillen, Michel |author5=Escorza, Ana|title=Establishing binarity amongst Galactic RV Tauri stars with a disc|journal=Astronomy & Astrophysics|volume=597|issue=|pages=A129, 18 pp.|date=January 2017|bibcode=2017A&A...597A.129M|doi=10.1051/0004-6361/201629125|arxiv=1610.00506}}
4. ^1 2 3 4 5 {{cite journal|author=Maas, T. |author2=Van Winckel, H. |author3=Waelkens, C.|title=RU Cen and SX Cen: Two strongly depleted RV Tauri stars in binary systems. The RV Tauri photometric b phenomenon and binarity|journal=Astronomy and Astrophysics|volume=386|issue=|pages=504–516|date=May 2002|bibcode=2002A&A...386..504M|doi=10.1051/0004-6361:20020209}}
5. ^1 2 3 {{cite journal|display-authors=etal|author=Arneson, R. A.|title=A SOFIA FORCAST Grism Study of the Mineralogy of Dust in the Winds of Proto-planetary Nebulae: RV Tauri Stars and SRd Variables|journal= The Astrophysical Journal|volume=843|issue=1|pages=article 51, 22 pp.|date=July 2017|bibcode=2017ApJ...843...51A|doi=10.3847/1538-4357/aa75cf|arxiv=1706.00445}}
6. ^1 2 3 4 5 6 {{cite journal|display-authors=etal|author=Deroo, P.|title=Resolving the compact dusty discs around binary post-AGB stars using N-band interferometry|journal=Astronomy and Astrophysics|volume=450|issue=1|pages=181–192|date=April 2006|bibcode=2006A&A...450..181D|doi=10.1051/0004-6361:20054300|arxiv=astro-ph/0601169}}
7. ^1 {{cite journal|display-authors=etal|author=Shenton, M.|title=Multiwavelength observations of RV Tauri stars. 4: SX Centauri|journal=Astronomy and Astrophysics|volume=292|issue=1|pages=102–114|date=December 1994|bibcode=1994A&A...292..102S|doi=}}
8. ^1 2 3 4 {{cite arXiv|eprint=1901.01409|last1=Bódi|first1=A.|title=Physical properties of galactic RV Tauri stars from Gaia DR2 data|last2=Kiss|first2=L. L.|class=astro-ph.SR|year=2019}}