Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F18%3A10385966" target="_blank" >RIV/00216208:11320/18:10385966 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/18:00494957 RIV/68378271:_____/18:00494957

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/201628363" target="_blank" >https://doi.org/10.1051/0004-6361/201628363</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201628363" target="_blank" >10.1051/0004-6361/201628363</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary

Popis výsledku v původním jazyce

V746 Cas is known to be a triple system composed of a close binary with an alternatively reported period of either 25.(d)4 or 27.(d)8 and a distant third component in a 170 yr (62 000 d) orbit. The object was also reported to exhibit multiperiodic light variations with periods from 0.(d)83 to 2.(d)50, on the basis of which it was classified as a slowly pulsating B star. Interest in further investigation of this system was raised by the recent detection of a variable magnetic field. Analysing spectra from four instruments, earlier published radial velocities, and several sets of photometric observations, we arrived at the following conclusions: (1) The optical spectrum is dominated by the lines of the B-type primary (T-eff 1 similar to 16 500(100) K), contributing 70% of the light in the optical region, and a slightly cooler B tertiary (T-eff 3 similar to 13 620(150) K). The lines of the low-mass secondary are below our detection threshold; we estimate that it could be a normal A or F star. (2) We resolved the ambiguity in the value of the inner binary period and arrived at a linear ephemeris of T-super.conj. = HJD 2 443 838.78(81) + 25.(d)41569(42) x E. (3) The intensity of the magnetic field undergoes a sinusoidal variation in phase with one of the known photometric periods, namely 2.(d)503867(19), which we identify with the rotational period of the tertiary. (4) The second dominant photometric 1.(d)0649524(40) period is tentatively identified with the rotational period of the broad-lined B-type primary, but this interpretation is much less certain and needs further verification. (5) If our interpretation of photometric periods is confirmed, the classification of the object as a slowly pulsating B star should be revised. (6) Applying an N-body model to different types of available observational data, we can constrain the orbital inclination of the inner orbit to similar to 60 degrees &lt; i(1) &lt; 85 degrees even in the absence of binary eclipses, and we estimate the probable properties of the triple system and its components.

Název v anglickém jazyce

Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary

Popis výsledku anglicky

V746 Cas is known to be a triple system composed of a close binary with an alternatively reported period of either 25.(d)4 or 27.(d)8 and a distant third component in a 170 yr (62 000 d) orbit. The object was also reported to exhibit multiperiodic light variations with periods from 0.(d)83 to 2.(d)50, on the basis of which it was classified as a slowly pulsating B star. Interest in further investigation of this system was raised by the recent detection of a variable magnetic field. Analysing spectra from four instruments, earlier published radial velocities, and several sets of photometric observations, we arrived at the following conclusions: (1) The optical spectrum is dominated by the lines of the B-type primary (T-eff 1 similar to 16 500(100) K), contributing 70% of the light in the optical region, and a slightly cooler B tertiary (T-eff 3 similar to 13 620(150) K). The lines of the low-mass secondary are below our detection threshold; we estimate that it could be a normal A or F star. (2) We resolved the ambiguity in the value of the inner binary period and arrived at a linear ephemeris of T-super.conj. = HJD 2 443 838.78(81) + 25.(d)41569(42) x E. (3) The intensity of the magnetic field undergoes a sinusoidal variation in phase with one of the known photometric periods, namely 2.(d)503867(19), which we identify with the rotational period of the tertiary. (4) The second dominant photometric 1.(d)0649524(40) period is tentatively identified with the rotational period of the broad-lined B-type primary, but this interpretation is much less certain and needs further verification. (5) If our interpretation of photometric periods is confirmed, the classification of the object as a slowly pulsating B star should be revised. (6) Applying an N-body model to different types of available observational data, we can constrain the orbital inclination of the inner orbit to similar to 60 degrees &lt; i(1) &lt; 85 degrees even in the absence of binary eclipses, and we estimate the probable properties of the triple system and its components.

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

2018

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

609

Číslo periodika v rámci svazku

Neuveden

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

20

Strana od-do

—

Kód UT WoS článku

000418963900005

EID výsledku v databázi Scopus

2-s2.0-85040233824