The symbiotic recurrent nova V3890 Sgr: binary parameters and pre-outburst activity. (arXiv:2104.06218v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mikolajewska_J/0/1/0/all/0/1">J. Mikolajewska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilkiewicz_K/0/1/0/all/0/1">K. Ilkiewicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galan_C/0/1/0/all/0/1">C. Galan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monard_B/0/1/0/all/0/1">B. Monard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Otulakowska_Hypka_M/0/1/0/all/0/1">M. Otulakowska-Hypka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shara_M/0/1/0/all/0/1">M. M. Shara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Udalski_A/0/1/0/all/0/1">A. Udalski</a>
We present and analyze optical photometry and high resolution SALT spectra of
the symbiotic recurrent nova V3890 Sgr at quiescence. The orbital period,
P=747.6 days has been derived from both photometric and spectroscopic data. Our
double-line spectroscopic orbits indicate that the mass ratio is
q=M_g/M_WD=0.78+/-0.05, and that the component masses are M_WD=1.35+/-0.13
Msun, and M_g=1.05+/-0.11 Msun. The orbit inclination is approximately 67-69
degr. The red giant is filling (or nearly filling) its Roche lobe, and the
distance set by its Roche lobe radius, d=9 kpc, is consistent with that
resulting from the giant pulsation period. The outburst magnitude of V3890 Sgr
is then very similar to those of RNe in the Large Magellanic Cloud. V3890 Sgr
shows remarkable photometric and spectroscopic activity between the nova
eruptions with timescales similar to those observed in the symbiotic recurrent
novae T CrB and RS Oph and Z And-type symbiotic systems. The active source has
a double-temperature structure which we have associated with the presence of an
accretion disc. The activity would be then caused by changes in the accretion
rate. We also provide evidence that V3890 Sgr contains a CO WD accreting at a
high, a few 1e-8 – 1e-7 Msun/yr, rate. The WD is growing in mass, and should
give rise to a Type Ia supernova within about 1,000,000 yrs – the expected
lifetime of the red giant.
We present and analyze optical photometry and high resolution SALT spectra of
the symbiotic recurrent nova V3890 Sgr at quiescence. The orbital period,
P=747.6 days has been derived from both photometric and spectroscopic data. Our
double-line spectroscopic orbits indicate that the mass ratio is
q=M_g/M_WD=0.78+/-0.05, and that the component masses are M_WD=1.35+/-0.13
Msun, and M_g=1.05+/-0.11 Msun. The orbit inclination is approximately 67-69
degr. The red giant is filling (or nearly filling) its Roche lobe, and the
distance set by its Roche lobe radius, d=9 kpc, is consistent with that
resulting from the giant pulsation period. The outburst magnitude of V3890 Sgr
is then very similar to those of RNe in the Large Magellanic Cloud. V3890 Sgr
shows remarkable photometric and spectroscopic activity between the nova
eruptions with timescales similar to those observed in the symbiotic recurrent
novae T CrB and RS Oph and Z And-type symbiotic systems. The active source has
a double-temperature structure which we have associated with the presence of an
accretion disc. The activity would be then caused by changes in the accretion
rate. We also provide evidence that V3890 Sgr contains a CO WD accreting at a
high, a few 1e-8 – 1e-7 Msun/yr, rate. The WD is growing in mass, and should
give rise to a Type Ia supernova within about 1,000,000 yrs – the expected
lifetime of the red giant.
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