Studying galactic novae systems at GMRT frequencies

N. G. Kantharia1*, G. C. Anupama, S. P. S. Eyres, N. Roy, T. P. Prabhu, N. M. Ashok, D. P. K. Banerjee, M. F. Bode, T. J. O’Brien, P. Dutta, S. Ramya and S. Bhatnagar
National Centre for Radio Astrophysics, TIFR, Pune 411007, India

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Galactic novae are binary systems consisting of a white dwarf and a companion star such as a main sequence star or a red giant. As the system evolves, the white dwarf accretes matter from the companion star which leads to a thermonuclear runaway igniting the matter on the white dwarf surface. This causes a sharp rise in the optical brightness of the system by a few to 15 magnitudes compared to quiescence. Several hundred Galactic novae are known and radio emission has been detected from about 33 of these with 9 showing the presence of non-thermal radio emission in their spectra. GMRT is optimal for detecting non-thermal emission from nova systems and has been used to observe about 11 systems to date. Radio continuum emission at frequencies < 1 GHz has been observed from two systems - GK Persei and RS Ophiuchi. We have now started a systematic programme to observe non-thermal radio emission from Galactic Novae called GNovaG which promises to add to the pool of multifrequency data and enhance our understanding of several outstanding questions related to nova progenitors and environment.

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