scholarly journals The Radio Properties of Symbiotic Stars

1988 ◽  
Vol 103 ◽  
pp. 69-75
Author(s):  
E.R. Seaquist
Keyword(s):  
Radio Emission ◽  
Symbiotic Stars ◽  
Bremsstrahlung Emission ◽  
Red Giant ◽  
Thermal Bremsstrahlung

AbstractRadio thermal bremsstrahlung emission has now been detected at centimeter wavelengths from about thirty symbiotic stars. These data combined with optical and IR data show that the radio emission in most systems may be understood in terms of the ionization of part of the wind of a red giant by a hot companion. The radio properties of symbiotic stars are reviewed and the agreement with and the limitations of this picture are examined.

scholarly journals The evolutionary status of symbiotic stars

1982 ◽  
Vol 70 ◽  
pp. 275-282 ◽  
Author(s):  
Bronislaw Rudak
Keyword(s):  
Cataclysmic Variables ◽  
Evolutionary Status ◽  
Spherically Symmetric ◽  
Symbiotic Stars ◽  
Transfer Phase ◽  
Common Envelope ◽  
Long Period ◽  
Red Giant ◽  
Detached Binaries ◽  
Rapid Mass

AbstractThe evolutionary relations between symbiotic stars and cataclysmic variables are presented. The symbiotic stars are assumed to be long period detached binaries containing a carbon-oxygen degenerate primary and a red giant losing its mass through a spherically symmetric wind. Such systems can be obtained in Case C evolution, provided a common envelope during a rapid mass transfer phase was not formed. The same way recurrent novae containing a red giant as a secondary component may be produced. The factors influencing the differences between symbiotic stars and nova-type stars are discussed.

scholarly journals Symbiotic Stars as Possible Progenitors of SNe Ia: Binary Parameters and Overall Outlook

2011 ◽  
Vol 7 (S281) ◽  
pp. 162-165 ◽  
Author(s):  
J. Mikołajewska
Keyword(s):  
White Dwarf ◽  
Physical Characteristics ◽  
Type Ia Supernovae ◽  
Symbiotic Stars ◽  
Type Ia ◽  
Red Giant ◽  
Ia Supernovae

AbstractSymbiotic stars are interacting binaries in which the first-formed white dwarf accretes and burns material from a red giant companion. This paper aims at presenting physical characteristics of these objects and discussing their possible link with progenitors of Type Ia supernovae.

scholarly journals Polarization of thermal bremsstrahlung emission due to electron pressure anisotropy

2016 ◽  
Vol 461 (2) ◽  
pp. 2162-2173 ◽  
Author(s):  
S. V. Komarov ◽  
I. I. Khabibullin ◽  
E. M. Churazov ◽  
A. A. Schekochihin
Keyword(s):  
Electron Pressure ◽  
Pressure Anisotropy ◽  
Bremsstrahlung Emission ◽  
Thermal Bremsstrahlung

Radio emission from symbiotic stars - A binary model

1984 ◽  
Vol 286 ◽  
pp. 263 ◽  
Author(s):  
A. R. Taylor ◽  
E. R. Seaquist
Keyword(s):  
Radio Emission ◽  
Symbiotic Stars ◽  
Binary Model

scholarly journals RADIO EMISSION FROM RED-GIANT HOT JUPITERS

2016 ◽  
Vol 820 (2) ◽  
pp. 122 ◽  
Author(s):  
Yuka Fujii ◽  
David S. Spiegel ◽  
Tony Mroczkowski ◽  
Jason Nordhaus ◽  
Neil T. Zimmerman ◽  
...  
Keyword(s):  
Radio Emission ◽  
Hot Jupiters ◽  
Red Giant

scholarly journals Miras Without Masers are Symbiotic Stars

1992 ◽  
Vol 135 ◽  
pp. 241-243
Author(s):  
B.M. Lewis
Keyword(s):  
Point Source ◽  
Accretion Disk ◽  
Symbiotic Stars ◽  
Natural Explanation ◽  
Giant Stars ◽  
Ir Stars ◽  
Circumstellar Shells ◽  
Red Giant ◽  
Point Source Catalog

AbstractAbout 40% of potential OH / IR stars, color selected from the IRAS Point Source Catalog, have no 1612 MHz masers. While these objects are rarely carbon rich, they are usually associated with circumstellar shells. The natural explanation for these “OH / IR star color mimics” is that they are systems with a degenerate companion collecting an accretion disk from a red giant wind. This provides them with an extra source of UV for dissociating their molecules. The persistent absence of the usual complement of masers from an O-rich shell is then a pointer to the presence of a degenerate companion. These occur in association with ~45% of old giant stars.

Relaxation Oscillations in Red-Giant Envelopes and the Symbiotic Stars

1973 ◽  
Vol 2 (4) ◽  
pp. 198-200 ◽  
Author(s):  
P. R. Wood
Keyword(s):  
Absorption Spectrum ◽  
Light Curves ◽  
Emission Lines ◽  
Symbiotic Star ◽  
Symbiotic Stars ◽  
Relaxation Oscillations ◽  
Cool Component ◽  
Cool Star ◽  
Red Giant ◽  
Eruptive Behaviour

The spectrum of a symbiotic star consists of an M-type absorption spectrum, a B-type shell spectrum and nebula emission lines, the relative contributions of these three components varying with time. The light curves of the symbiotic stars vary with a semi-regular period typically 200-800 days while larger eruptions occur on a timescale of ~ 3.5 years. Some suggestions which have been advanced to explain the combination spectrum, variability and eruptive behaviour of the symbiotic stars are: (a)the symbiotic stars are binaries consisting of a hot and cool component.(b)the symbiotic stars consist of a single hot star surrounded by a large optically thick envelope giving the appearance of a hot continuum with the absorption spectrum of a cool star superimposed on it.(c)the symbiotic stars are single stars surrounded by a shock wave heated chromosphere.Although some of the symbiotic stars are undoubtedly binaries (for example, T Coronae Borealis), observatienal evidence suggests that others may be explained by hypothesis (c) above. The calculations described below provide an explanation of the symbiotic stars in conjunction with hypothesis (c).

scholarly journals Properties Of Cool Stellar Components in S-Type Symbiotic Stars

1988 ◽  
Vol 103 ◽  
pp. 37-41
Author(s):  
O.G. Taranova ◽  
B.P. Yudin
Keyword(s):  
Spectral Type ◽  
Dust Emission ◽  
Roche Lobe ◽  
Red Giants ◽  
Symbiotic Stars ◽  
Cool Component ◽  
Cool Star ◽  
Type D ◽  
Red Giant

In 1975 Webster and Allen (1975) divided all symbiotic stars into two groups-those in which the 1-4μm continuum show only the presence of a cool star (type S),and those in which dust emission dominates (type D). With the exception of some of yellow symbiotic stars, the dust presence in others correlates with the spectral type of their cool components. That is why one can say that S-type symbiotics contain red giants with spectral type earlier than M6-M7.At the IAU Colloq. N 7Q Allen (1982) noted that it is difficult to escape the conclusion that symbiotic stars contain normal cool giants. Nowadays it is certaiu to be correct because the modern observations of S-type symbiotic stars have not yet discovered any specific distinctions between their cool stellar components and normal red giants. At the same time it should be noted that some of these, for example, Z And, CI Cyg may be interacting binaries in which the cool component apparently fields its Roche lobe and unstable accretion of gas from the red giant onto its hot companion leads to the out bursts of the latter (Kenyon and Webbink 1984; Yudin 1987).

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