Modeling spectra of MN112. (arXiv:2009.13463v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Kostenkov_A/0/1/0/all/0/1">A. Kostenkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabrika_S/0/1/0/all/0/1">S. Fabrika</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sholukhova_O/0/1/0/all/0/1">O. Sholukhova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkisyan_A/0/1/0/all/0/1">A. Sarkisyan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bizyaev_D/0/1/0/all/0/1">D. Bizyaev</a>
MN112 is the Galactic luminous blue variable (LBV) candidate with
circumstellar nebula. P Cygni is the first discovered LBV, which was recorded
during major eruptions in the 17th century. The stars have similar spectra with
strong emission hydrogen lines, He I, N II, Si II, and Fe III lines. We present
results of the spectroscopic analysis and modeling of MN112 spectra. We
obtained main stellar parameters and chemical abundances of MN112 and compared
them with those of P Cygni. Atmosphere models were calculated using non-LTE
radiative transfer code CMFGEN. We have used spectra of MN112 obtained with the
3.5-m telescope at the Observatory of Calar Alto and 3.5-m ARC telescope at the
Apache Point Observatory. P Cygni spectra were taken with the 6-m BTA
telescope. We have found the best-fit of the observed spectrum with the model
at temperature $T_{text{eff}}= 15,200$K, clumping-corrected mass-loss rate
$dot{M}f^{-0.5}=5.74 times 10^{-5}, M_{odot}text{yr}^{-1}$, filling-factor
$f=0.1$, luminosity $L=5.77 times 10^5, L_{odot}$ for MN112. The ratio of
helium to hydrogen He/H is 0.37 (by the number of atoms) with nitrogen
overabundance ($X_text{N}/ X_{odot} = 6.8$) and the underabundance of carbon
($X_text{C}/ X_{odot} < 0.1$).
MN112 is the Galactic luminous blue variable (LBV) candidate with
circumstellar nebula. P Cygni is the first discovered LBV, which was recorded
during major eruptions in the 17th century. The stars have similar spectra with
strong emission hydrogen lines, He I, N II, Si II, and Fe III lines. We present
results of the spectroscopic analysis and modeling of MN112 spectra. We
obtained main stellar parameters and chemical abundances of MN112 and compared
them with those of P Cygni. Atmosphere models were calculated using non-LTE
radiative transfer code CMFGEN. We have used spectra of MN112 obtained with the
3.5-m telescope at the Observatory of Calar Alto and 3.5-m ARC telescope at the
Apache Point Observatory. P Cygni spectra were taken with the 6-m BTA
telescope. We have found the best-fit of the observed spectrum with the model
at temperature $T_{text{eff}}= 15,200$K, clumping-corrected mass-loss rate
$dot{M}f^{-0.5}=5.74 times 10^{-5}, M_{odot}text{yr}^{-1}$, filling-factor
$f=0.1$, luminosity $L=5.77 times 10^5, L_{odot}$ for MN112. The ratio of
helium to hydrogen He/H is 0.37 (by the number of atoms) with nitrogen
overabundance ($X_text{N}/ X_{odot} = 6.8$) and the underabundance of carbon
($X_text{C}/ X_{odot} < 0.1$).
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