Abstract From the HeII λ1640 emission line equivalent width values in all good available IUE low resolution spectra, we have deduced the correspondent mass accretion rate values Ṁ for SS Cygni, using the optically thick boundary-layer model by Patterson and Raymond 1985. The Ṁ behaviour can be distinguished as follows: 1) in the rising and declining phase of an outburst, Ṁ is not inconsistent with the commonly accepted theoretical models on the quiescence-outburst optical behaviour of dwarf novae, which suppose the luminosity depending only on the rate Ṁ at which matter is accreted; 2) Ṁ in outburst is < M ̇ in quiscence and suggests that the accretion is not the only energy release mechanism responsible for the higher luminosity. In this paper we will discuss the results searching for alternative and/or additive mechanism in producing the highest luminosities associated with the outbursts.


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    Title :

    SS Cygni: The mass accretion rate behaviour in quiescence and in outburst


    Contributors:
    Gaudenzi, S. (author) / Lombardi, R. (author) / Giovannelli, F. (author) / Claudi, R. (author)

    Published in:

    Advances in Space Research ; 8 , 2-3 ; 325-327


    Publication date :

    1988-01-01


    Size :

    3 pages




    Type of media :

    Article (Journal)


    Type of material :

    Electronic Resource


    Language :

    English



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