New insights on the massive interacting binary UU Cassiopeiae

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10423258" target="_blank" >RIV/00216208:11320/20:10423258 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=B6eIe_ToSM" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=B6eIe_ToSM</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202038938" target="_blank" >10.1051/0004-6361/202038938</a>

Jazyk výsledku

angličtina

Název v původním jazyce

New insights on the massive interacting binary UU Cassiopeiae

Popis výsledku v původním jazyce

We present the results of our study of the close binary UU Cassiopeiae based on previously published multiwavelength photometric and spectroscopic data. Based on eclipse timings from the last 117 years, we find an improved orbital period of Po = 8d : 519296(8). In addition, we find a long cycle of length T similar to 270 d in the Ic-band data. There is no evidence for orbital period change over the last century, suggesting that the rate of mass loss from the system or mass exchange between the stars is small. Sporadic and rapid brightness drops of up to Delta V = 0:3 mag are detected throughout the orbital cycle, and infrared photometry clearly suggests the presence of circumstellar matter. We model the orbital light curve of 11 published datasets, fixing the mass ratio and cooler star temperature from previous spectroscopic work: q = 0.52 and Tc = 22 700 K. We find a system seen at an angle of 74ffi with a stellar separation of 52 R fi, a temperature for the hotter star of Th = 30 200K and, for the hotter and cooler stars, respectively, stellar masses of 17.4 and 9 M fi, radii of 7.0 and 16.9 R fi, and surface gravities log g = 3.98 and 2.94. We find an accretion disk surrounding the more massive star that has a radius of 21 R fi and a vertical thickness at its outer edge of 6.5 R fi; the disk nearly occults the hotter star. Two active regions hotter than the surrounding disk are found, one located roughly in the expected position where the stream impacts the disk and the other on the opposite side of the disk. Changes are observed in parameters of the disk and spots in di fferent datasets.

Název v anglickém jazyce

New insights on the massive interacting binary UU Cassiopeiae

Popis výsledku anglicky

We present the results of our study of the close binary UU Cassiopeiae based on previously published multiwavelength photometric and spectroscopic data. Based on eclipse timings from the last 117 years, we find an improved orbital period of Po = 8d : 519296(8). In addition, we find a long cycle of length T similar to 270 d in the Ic-band data. There is no evidence for orbital period change over the last century, suggesting that the rate of mass loss from the system or mass exchange between the stars is small. Sporadic and rapid brightness drops of up to Delta V = 0:3 mag are detected throughout the orbital cycle, and infrared photometry clearly suggests the presence of circumstellar matter. We model the orbital light curve of 11 published datasets, fixing the mass ratio and cooler star temperature from previous spectroscopic work: q = 0.52 and Tc = 22 700 K. We find a system seen at an angle of 74ffi with a stellar separation of 52 R fi, a temperature for the hotter star of Th = 30 200K and, for the hotter and cooler stars, respectively, stellar masses of 17.4 and 9 M fi, radii of 7.0 and 16.9 R fi, and surface gravities log g = 3.98 and 2.94. We find an accretion disk surrounding the more massive star that has a radius of 21 R fi and a vertical thickness at its outer edge of 6.5 R fi; the disk nearly occults the hotter star. Two active regions hotter than the surrounding disk are found, one located roughly in the expected position where the stream impacts the disk and the other on the opposite side of the disk. Changes are observed in parameters of the disk and spots in di fferent datasets.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA17-00871S" target="_blank" >GA17-00871S: Vlastnosti circumstelární látky u B[e] hvězd</a><br>

Návaznosti

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

Rok uplatnění

2020

Kód důvěrnosti údajů

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

Název periodika

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

—

Svazek periodika

642

Číslo periodika v rámci svazku

říjen

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

9

Strana od-do

A211

Kód UT WoS článku

000586582900003

EID výsledku v databázi Scopus

2-s2.0-85094876109