A Spectroscopic Orbit for the Late-type Be Star beta CMi

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10369295" target="_blank" >RIV/00216208:11320/17:10369295 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.3847/1538-4357/836/1/112" target="_blank" >http://dx.doi.org/10.3847/1538-4357/836/1/112</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/836/1/112" target="_blank" >10.3847/1538-4357/836/1/112</a>

Jazyk výsledku

angličtina

Název v původním jazyce

A Spectroscopic Orbit for the Late-type Be Star beta CMi

Popis výsledku v původním jazyce

The late-type Be star beta CMi is remarkably stable compared to other Be stars that have been studied. This has led to a realistic model of the outflowing Be disk by Klement et al. These results showed that the disk is likely truncated at a finite radius from the star, which Klement et al. suggest is evidence for an unseen binary companion in orbit. Here we report on an analysis of the Ritter Observatory spectroscopic archive of a CMi to search for evidence of the elusive companion. We detect periodic Doppler shifts in the wings of the Ha line with a period of 170 days and an amplitude of 2.25 km s(-1) , consistent with a low-mass binary companion (M approximate to 0.42M circle dot). We then compared small changes in the violet-to-red peak height changes (V/R) with the orbital motion. We find weak evidence that it does follow the orbital motion, as suggested by recent Be binary models by Panoglou et al. Our results, which are similar to those for several other Be stars, suggest that beta CMi may be a product of binary evolution where Roche lobe overflow has spun up the current Be star, likely leaving a hot subdwarf or white dwarf in orbit around the star. Unfortunately, no direct sign of this companion star is found in the very limited archive of International Ultraviolet Explorer spectra.

Název v anglickém jazyce

A Spectroscopic Orbit for the Late-type Be Star beta CMi

Popis výsledku anglicky

The late-type Be star beta CMi is remarkably stable compared to other Be stars that have been studied. This has led to a realistic model of the outflowing Be disk by Klement et al. These results showed that the disk is likely truncated at a finite radius from the star, which Klement et al. suggest is evidence for an unseen binary companion in orbit. Here we report on an analysis of the Ritter Observatory spectroscopic archive of a CMi to search for evidence of the elusive companion. We detect periodic Doppler shifts in the wings of the Ha line with a period of 170 days and an amplitude of 2.25 km s(-1) , consistent with a low-mass binary companion (M approximate to 0.42M circle dot). We then compared small changes in the violet-to-red peak height changes (V/R) with the orbital motion. We find weak evidence that it does follow the orbital motion, as suggested by recent Be binary models by Panoglou et al. Our results, which are similar to those for several other Be stars, suggest that beta CMi may be a product of binary evolution where Roche lobe overflow has spun up the current Be star, likely leaving a hot subdwarf or white dwarf in orbit around the star. Unfortunately, no direct sign of this companion star is found in the very limited archive of International Ultraviolet Explorer spectra.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

—

Svazek periodika

836

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

5

Strana od-do

—

Kód UT WoS článku

000397304500064

EID výsledku v databázi Scopus

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