Classical Nova Persei 2018 outburst from the dwarf nova V392 Per. (arXiv:2007.13337v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Chochol_D/0/1/0/all/0/1">Drahomír Chochol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shugarov_S/0/1/0/all/0/1">Sergey Shugarov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hambalek_L/0/1/0/all/0/1">Ľubomír Hambálek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Skopal_A/0/1/0/all/0/1">Augustin Skopal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parimucha_S/0/1/0/all/0/1">Štefan Parimucha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubovsky_P/0/1/0/all/0/1">Pavol Dubovský</a>
On 2018, April 29, a bright classical nova (CN) Per 2018 was discovered. Its
progenitor is a well-known dwarf nova V392 Per. In this contribution, we
analyze $UBVR_{C}I_{C}$ photometry and optical spectroscopy of the CN V392 Per.
From the $V$ light curve (LC) we found the brightness decline times t$_{2,V}$ =
3 d, t$_{3,V}$ = 10 d and calculated absolute magnitude of the nova at maximum
$MV_{max}$ = -9.30 ${pm}$0.57 using the new $MV_{max}$ – t$_{3}$ “universal”
decline law and $MV_{15}$ relations, adopting the Gaia data for CNe. We
determined the colour excess $E_{B-V}$ = 0.90$pm$0.09 and distance to the nova
$d$ = 3.55$pm$0.6 kpc. The optical spectrum obtained in brightness maximum
resembles that of the F2 supergiant. Its bolometric luminosity computed by
fitting the continuum by atmospheric and black-body models is in agreement with
the luminosity, that we have found from photometry. We estimated the mass of
the ONe white dwarf in V392 Per as $M_{wd}$ = 1.21 M$_{odot}$. The CN Per 2018
can be classified as a fast super-Eddington nova with an outburst LC of plateau
type. Nova displayed He/N spectrum classification, large expansion velocities,
and triple-peaked emission-line profiles during the decline, explained by
equatorial ring seen nearly face on and a bipolar flow aligned almost with the
line of sight. The post maximum spectra of CN Per 2018 and available radio data
were used to estimate the inclination angle of the system as $isim$
9$^{circ}$. The difference in intensity of redward and blueward emission bumps
is possible to explain by about 1.5 times higher density of the receding
outtflow. The rapid increase of the bipolar outflow radial velocities by
$sim$300 km/s around day 5 after the maximum was caused by the fast bipolar
winds from the burning white dwarf after shrinking of its pseudophotosphere.
On 2018, April 29, a bright classical nova (CN) Per 2018 was discovered. Its
progenitor is a well-known dwarf nova V392 Per. In this contribution, we
analyze $UBVR_{C}I_{C}$ photometry and optical spectroscopy of the CN V392 Per.
From the $V$ light curve (LC) we found the brightness decline times t$_{2,V}$ =
3 d, t$_{3,V}$ = 10 d and calculated absolute magnitude of the nova at maximum
$MV_{max}$ = -9.30 ${pm}$0.57 using the new $MV_{max}$ – t$_{3}$ “universal”
decline law and $MV_{15}$ relations, adopting the Gaia data for CNe. We
determined the colour excess $E_{B-V}$ = 0.90$pm$0.09 and distance to the nova
$d$ = 3.55$pm$0.6 kpc. The optical spectrum obtained in brightness maximum
resembles that of the F2 supergiant. Its bolometric luminosity computed by
fitting the continuum by atmospheric and black-body models is in agreement with
the luminosity, that we have found from photometry. We estimated the mass of
the ONe white dwarf in V392 Per as $M_{wd}$ = 1.21 M$_{odot}$. The CN Per 2018
can be classified as a fast super-Eddington nova with an outburst LC of plateau
type. Nova displayed He/N spectrum classification, large expansion velocities,
and triple-peaked emission-line profiles during the decline, explained by
equatorial ring seen nearly face on and a bipolar flow aligned almost with the
line of sight. The post maximum spectra of CN Per 2018 and available radio data
were used to estimate the inclination angle of the system as $isim$
9$^{circ}$. The difference in intensity of redward and blueward emission bumps
is possible to explain by about 1.5 times higher density of the receding
outtflow. The rapid increase of the bipolar outflow radial velocities by
$sim$300 km/s around day 5 after the maximum was caused by the fast bipolar
winds from the burning white dwarf after shrinking of its pseudophotosphere.
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