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An RS Canum Venaticorum variable is a type of variable star. The variable type consists of close binary stars[1] having active chromospheres which can cause large stellar spots. These spots are believed to cause variations in their observed luminosity. Systems can exhibit variations on timescales of years due to variation in the spot surface coverage fraction, as well as periodic variations which are, in general, close to the orbital period of the binary system. Some systems exhibit variations in luminosity due to their being eclipsing binaries. Typical brightness fluctuation is around 0.2 magnitudes. They take their name from the star RS Canum Venaticorum (abbreviated RS CVn).
Otto Struve (1946) first called attention to the group, but it was Oliver (1974) who was the first to formally propose a set of observational characteristics to define the RS CVn criteria. The working definition, as it is used today, was that set down by Hall (1976).[2][1]
The RS CVn systems are divided into five separate subgroups:
- Regular systems. Orbital periods are between 1 and 14 days. The hotter component is of the spectral type F or G and luminosity class V or IV. Strong Ca II H and K emission is seen outside eclipse.
- Short period systems. Components are detached and orbital periods are less than 1 day. The hotter component is of the spectral type F or G and luminosity class V or IV. Ca II H and K emission is displayed in one or both components.
- Long period systems. Orbital periods is greater than 14 days. Either component is of the spectral type G through K and luminosity class II through IV. Strong Ca II H and K emission is seen outside eclipse.
- Flare star systems. In this case the hotter component is of the spectral type dKe or dMe, where the emission refers to strong Ca II H and K.
- V471 Tau type systems. The hotter component is a white dwarf. The cooler component, spectral class G through K, displays strong Ca II H and K emission.
![Visual band light curves for RS Canum Venaticorum, adapted from Rodonò et al. (1995)[3]](http://upload.wikimedia.org/wikipedia/commons/thumb/4/4b/RSCVnLightCurve.png/220px-RSCVnLightCurve.png)
The light curves of RS CVn type systems show a peculiar semiperiodic structure outside eclipse. This structure has been referred to as a distortion wave in the light curve. Eaton and Hall (1979) determined that the simplest mechanism for the creation of the distortion wave was "starspots", which, in analogy to sunspots, are large, cool active regions on the photosphere. Such spots have since been observed indirectly[4] on many systems.
Chromospheric activity is signaled by the presence of emission cores in the Ca II H and K resonance lines. Balmer emission, or Hα, is also associated with active chromospheres. X-ray emission is known as a tracer for active coronal regions, and ultraviolet (UV) emission and flaring are, by solar analogy, known to be associated with stellar active and transition regions. These areas on the Sun are associated with intense magnetic fields, and sunspot activity is enhanced in and around these magnetically active regions.
Some RS CVn type stars are known X-ray and radio emitters. The radio emission is nonthermal in origin (gyrosynchrotron) and is one of the few direct indicators of magnetic fields. The X-ray luminosities are on the order of Lx >> 1024 watts. This emission has been interpreted, in solar analogy, as being caused by a hot, T ~ 107 K, corona.
Another subgroup of RS CVns is known to have infrared excess emission, seen by the Spitzer Space Telescope[5]
Notes
- Berdyugina 2.4 RS CVn stars
- Hall, Douglas S. (1976). "The RS CVN Binaries and Binaries with Similar Properties". International Astronomical Union Colloquium. 29: 287–348. doi:10.1017/S0252921100062011.
- Rodonò, M.; Lanza, A. F.; Catalano, S. (September 1995). "Starspot evolution, activity cycle and orbital period variation of the prototype active binary RS Canum Venaticorum". Astronomy and Astrophysics. 301: 75–88. Retrieved 19 December 2021.
- Cameron Eclipse movies showing spots in XY Ursae Majoris binary
- Matranga, M., Drake, J.J., Kashyap, V.L., Marengo, M., & Kuchner, M.J. 2010, Astrophysical Journal
References
- Cameron, Andrew Collier. "Mapping starspots and magnetic fields on cool stars". University of St Andrews. Retrieved 2008-08-28. (explains how Doppler imaging works)
- Berdyugina, Svetlana V. (2005). "Starspots: A Key to the Stellar Dynamo". Living Reviews in Solar Physics. Institute of Astronomy ETHZ, Max Planck Society. 2 (8): 8. Bibcode:2005LRSP....2....8B. doi:10.12942/lrsp-2005-8. Retrieved 2008-08-28.
Further reading
 | This article includes a list of general references, but it lacks sufficient corresponding inline citations. (April 2009) |
- Eaton,J.A. and Hall,D.S. 1979, Astrophys. Jour., 227, 907.
- Hall,D.S. 1976, in IAU Colloquium No. 29, "Multiple Periodic Variable Stars" (D. Reidel: Boston), p. 278-348.
- Oliver,J.P. 1974, Ph.D. Dissertation, University of California at Los Angeles.
- Samus N.N., Durlevich O.V., et al. Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.)
- Struve,O. 1946, Ann. d'Astrophys, 9, 1.
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| Eclipsing |
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На других языках
[de] RS-Canum-Venaticorum-Stern
RS-Canum-Venaticorum-Sterne sind eine Klasse von getrennten Doppelsternen, bestehend aus massereicheren primären Riesen oder Unterriesen mit einem Spektraltyp G bis K und einem Begleiter, der ein Unterriese oder Hauptreihenstern vom Spektraltyp G bis M ist. RS-CVn-Sterne zeigen außerhalb eines möglichen Bedeckungslichtwechsels eine Modulation der Lichtkurve mit einer Amplitude von bis 0,6 mag in V, die als eine Rotation von Sternflecken auf der Oberfläche der Sterne interpretiert wird. Die ausgeprägte magnetische Aktivität dieser Sterne zeigt sich durch eine heiße Korona im Bereich der Röntgenstrahlung sowie die Beobachtungen von Flares[1].- [en] RS Canum Venaticorum variable
[es] Estrella variable RS Canum Venaticorum
Las estrellas variables RS Canum Venaticorum o estrellas RS CVn son un tipo de variables eruptivas compuestas por un estrella binaria cuyas componentes, de tipo espectral F, G o K, tienen intensa actividad cromosférica. Ambas estrellas están muy próximas, con un período orbital típico de unos pocos días a 20 días. Las variaciones de brillo suelen ser del orden de 0,2 magnitudes y son debidas a manchas estelares análogas a las del Sol, pero de dimensiones descomunales, ya que oscurecen un porcentaje importante de la estrella. Estas manchas o regiones de menor temperatura giran con un período similar al período orbital del sistema binario. Sobrepuesto a este período corto existen períodos más largos de actividad cromosférica, similares al ciclo solar, que pueden durar de 1 a 4 años. Estas estrellas también son importantes radiofuentes y emisoras de rayos X.[ru] Переменная типа RS Гончих Псов
Переменные типа RS Гончих Псов (RS Canum Venaticorum, RS CVn) — эруптивные переменные звёзды. К этому типу относятся тесные двойные системы с эмиссией Н и К Ca II в спектре, компоненты которых обладают повышенной хромосферной активностью, вызывающей квазипериодическую переменность их блеска с периодом, близким к периоду обращения, и переменной амплитудой, обычно достигающей 0.2m.Другой контент может иметь иную лицензию. Перед использованием материалов сайта WikiSort.org внимательно изучите правила лицензирования конкретных элементов наполнения сайта.
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