New insights on the massive interacting binary UU Cassiopeiae

Result code in 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>

Result on the web

<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>

Result language

angličtina

Original language name

New insights on the massive interacting binary UU Cassiopeiae

Original language description

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.

Czech name

—

Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GA17-00871S" target="_blank" >GA17-00871S: Properties of the circumstellar matter around B[e] stars</a><br>

Continuities

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

Publication year

2020

Confidentiality

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

Name of the periodical

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

—

Volume of the periodical

642

Issue of the periodical within the volume

říjen

Country of publishing house

FR - FRANCE

Number of pages

9

Pages from-to

A211

UT code for WoS article

000586582900003

EID of the result in the Scopus database

2-s2.0-85094876109