Connection between the long secondary period and red giant evolution

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F21%3A10438306" target="_blank" >RIV/00216208:11320/21:10438306 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Na7vMKJiNm" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=Na7vMKJiNm</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202038642" target="_blank" >10.1051/0004-6361/202038642</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Connection between the long secondary period and red giant evolution

Popis výsledku v původním jazyce

Aims. The mechanism behind the long secondary period (LSP) observed in pulsating red giants remains unknown. In this work, I investigate the connection between the red giant branch and the asymptotic giant branch evolution and the appearance of the LSP - a phenomenon that has been observed in a significant proportion of red giants.Methods. For the purposes of this work, I used the OGLE-III sample of the OSARG variables in the Large Magellanic Cloud. I constructed density maps in the period-luminosity as well as color-magnitude planes for the stars showing an LSP and compared them to the remaining giants. I also fit the spectral energy distribution to test whether an additional source of reddening is present in the LSP stars.Results. Here, I posit the hypothesis that the LSP phenomenon may be related to a transition between the different pulsation period-luminosity sequences. I also show that an overabundance of the stars showing LSP can be observed around the tip of the red giant branch, and much more prominently, at the upper part of the asymptotic giant branch. The main over-density region appears to be slightly fainter and redder than the bulk of the asymptotic giant branch. It also seems to correspond to the area of the Hertzsprung-Russell diagram where stable winds and high mass loss are present.Conclusions. The LSP can possibly be shown to be a recurring phenomenon that appears and disappears at various points of the red giant evolution. The LSP stars appear to be more reddened than other giants, which suggests the intrinsic nature of the reddening is likely to be related to large dust emission. The analysis appears to confirm the hypothesis that there is a relation between the mass loss due to the presence of strong stellar wind and the appearance of an LSP.

Název v anglickém jazyce

Connection between the long secondary period and red giant evolution

Popis výsledku anglicky

Aims. The mechanism behind the long secondary period (LSP) observed in pulsating red giants remains unknown. In this work, I investigate the connection between the red giant branch and the asymptotic giant branch evolution and the appearance of the LSP - a phenomenon that has been observed in a significant proportion of red giants.Methods. For the purposes of this work, I used the OGLE-III sample of the OSARG variables in the Large Magellanic Cloud. I constructed density maps in the period-luminosity as well as color-magnitude planes for the stars showing an LSP and compared them to the remaining giants. I also fit the spectral energy distribution to test whether an additional source of reddening is present in the LSP stars.Results. Here, I posit the hypothesis that the LSP phenomenon may be related to a transition between the different pulsation period-luminosity sequences. I also show that an overabundance of the stars showing LSP can be observed around the tip of the red giant branch, and much more prominently, at the upper part of the asymptotic giant branch. The main over-density region appears to be slightly fainter and redder than the bulk of the asymptotic giant branch. It also seems to correspond to the area of the Hertzsprung-Russell diagram where stable winds and high mass loss are present.Conclusions. The LSP can possibly be shown to be a recurring phenomenon that appears and disappears at various points of the red giant evolution. The LSP stars appear to be more reddened than other giants, which suggests the intrinsic nature of the reddening is likely to be related to large dust emission. The analysis appears to confirm the hypothesis that there is a relation between the mass loss due to the presence of strong stellar wind and the appearance of an LSP.

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/LTAUSA18093" target="_blank" >LTAUSA18093: Časová proměnnost v astronomii: účast v projektu All-Sky Automated Survey for Supernovae</a><br>

Návaznosti

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

Rok uplatnění

2021

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

649

Číslo periodika v rámci svazku

May

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

9

Strana od-do

A110

Kód UT WoS článku

000658514700004

EID výsledku v databázi Scopus

2-s2.0-85106913934