New outburst of the symbiotic nova AG Pegasi after 165 yr

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10371670" target="_blank" >RIV/00216208:11320/17:10371670 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201629593" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201629593</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201629593" target="_blank" >10.1051/0004-6361/201629593</a>

Jazyk výsledku

angličtina

Název v původním jazyce

New outburst of the symbiotic nova AG Pegasi after 165 yr

Popis výsledku v původním jazyce

Context. AG Peg is known as the slowest symbiotic nova, which experienced its nova-like outburst around 1850. After 165 yr, during June of 2015, it erupted again showing characteristics of the Z And-type outburst. Aims. The primary objective is to determine basic characteristics, the nature and type of the 2015 outburst of AG Peg. Methods. We achieved this aim by modelling the spectral energy distribution using low-resolution spectroscopy (330-750 nm; R = 500-1000), medium-resolution spectroscopy (420-720 nm; R similar to 11 000), and UBVRCIC photometry covering the 2015 outburst with a high cadence. Optical observations were complemented with the archival HST and FUSE spectra from the preceding quiescence. Results. During the outburst, the luminosity of the hot component was in the range of 2-11 x 10(37) (d/0.8 kpc)(2) erg s(-1), being in correlation with the light curve (LC) profile. To generate the maximum luminosity by the hydrogen burning, the white dwarf (WD) had to accrete at similar to 3 x 10(-7) M-circle dot yr(-1), which exceeds the stable-burning limit and thus led to blowing optically thick wind from the WD. We determined its mass-loss rate to a few x10(-6) M-circle dot yr(-1). At the high temperature of the ionising source, 1.5-2.3 x 10(5) K, the wind converted a fraction of the WD&apos;s photospheric radiation into the nebular emission that dominated the optical. A one order of magnitude increase of the emission measure, from a few x10(59) (d/0.8 kpc)(2) cm(-3) during quiescence, to a few x10(60) (d/0.8 kpc)(2) cm(-3) during the outburst, caused a 2 mag brightening in the LC, which is classified as the Z And-type of the outburst. Conclusions. The very high nebular emission and the presence of a disk-like H i region encompassing the WD, as indicated by a significant broadening and high flux of the Raman-scattered O VI 6825 angstrom line during the outburst, is consistent with the ionisation structure of hot components in symbiotic stars during active phases.

Název v anglickém jazyce

New outburst of the symbiotic nova AG Pegasi after 165 yr

Popis výsledku anglicky

Context. AG Peg is known as the slowest symbiotic nova, which experienced its nova-like outburst around 1850. After 165 yr, during June of 2015, it erupted again showing characteristics of the Z And-type outburst. Aims. The primary objective is to determine basic characteristics, the nature and type of the 2015 outburst of AG Peg. Methods. We achieved this aim by modelling the spectral energy distribution using low-resolution spectroscopy (330-750 nm; R = 500-1000), medium-resolution spectroscopy (420-720 nm; R similar to 11 000), and UBVRCIC photometry covering the 2015 outburst with a high cadence. Optical observations were complemented with the archival HST and FUSE spectra from the preceding quiescence. Results. During the outburst, the luminosity of the hot component was in the range of 2-11 x 10(37) (d/0.8 kpc)(2) erg s(-1), being in correlation with the light curve (LC) profile. To generate the maximum luminosity by the hydrogen burning, the white dwarf (WD) had to accrete at similar to 3 x 10(-7) M-circle dot yr(-1), which exceeds the stable-burning limit and thus led to blowing optically thick wind from the WD. We determined its mass-loss rate to a few x10(-6) M-circle dot yr(-1). At the high temperature of the ionising source, 1.5-2.3 x 10(5) K, the wind converted a fraction of the WD&apos;s photospheric radiation into the nebular emission that dominated the optical. A one order of magnitude increase of the emission measure, from a few x10(59) (d/0.8 kpc)(2) cm(-3) during quiescence, to a few x10(60) (d/0.8 kpc)(2) cm(-3) during the outburst, caused a 2 mag brightening in the LC, which is classified as the Z And-type of the outburst. Conclusions. The very high nebular emission and the presence of a disk-like H i region encompassing the WD, as indicated by a significant broadening and high flux of the Raman-scattered O VI 6825 angstrom line during the outburst, is consistent with the ionisation structure of hot components in symbiotic stars during active phases.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2017

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy &amp; Astrophysics [online]

ISSN

1432-0746

e-ISSN

—

Svazek periodika

604

Číslo periodika v rámci svazku

srpen

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

19

Strana od-do

—

Kód UT WoS článku

000408480100014

EID výsledku v databázi Scopus

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