LAMOST J040901.83+329355.6-a new Galactic star with Wolf-Rayet characteristics in the transitional stage from post-asymptotic giant branch to central star of a planetary nebula

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00582368" target="_blank" >RIV/67985815:_____/23:00582368 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68378271:_____/23:00582368

Výsledek na webu

<a href="https://hdl.handle.net/11104/0353356" target="_blank" >https://hdl.handle.net/11104/0353356</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stad3960" target="_blank" >10.1093/mnras/stad3960</a>

Jazyk výsledku

angličtina

Název v původním jazyce

LAMOST J040901.83+329355.6-a new Galactic star with Wolf-Rayet characteristics in the transitional stage from post-asymptotic giant branch to central star of a planetary nebula

Popis výsledku v původním jazyce

The similarity in physical conditions in the winds of low-mass post-asymptotic giant branch stars and evolved massive stars leads to the appearance of an interesting phenomenon of spectral mimicry. Because of this, the discovery of every new star with a Wolf-Rayet (WR) spectrum requires a special study of its evolutionary status before it can be included in the list of Galactic WR stars. A couple of years ago, LAMOST J040901.83+323955.6 (hereafter J0409+3239) was selected as a WR star in the LAMOST spectroscopic data base by machine-learning methods. In this work, we investigate its evolutionary status. After analysing the spatial location of J0409+3239 in the Galaxy and its position in the colour-magnitude diagram, we conclude that J0409+3239 is instead a low-mass object displayng the WR phenomenon. Its luminosity is L-*=1000 L circle dot and its effective temperature is T-eff = 40 000 K. Using new and archival photometric data, we detected irregular variability on time-scales from hours to tens of days with an amplitude of up to similar to 0.2 mag. A comparison of the spectrum obtained in 2022 with that from 2014 also shows evidence of spectral variability. The absence of a clearly detected circumstellar nebula prevents the classification of J0409+3239 as [WR], namely as the central star of a planetary nebula (CSPN). However, the position of J0409+3239 on the Hertzsprung-Russell diagram suggests that this object is a low-mass star caught in a rare transitional phase to CSPN. Estimation of the J0409+3239 mass based on evolutionary tracks shows that it is less than 0.9 M circle dot, and thus that the age of the Galaxy is barely sufficient for the star to have evolved to its current stage.

Název v anglickém jazyce

LAMOST J040901.83+329355.6-a new Galactic star with Wolf-Rayet characteristics in the transitional stage from post-asymptotic giant branch to central star of a planetary nebula

Popis výsledku anglicky

The similarity in physical conditions in the winds of low-mass post-asymptotic giant branch stars and evolved massive stars leads to the appearance of an interesting phenomenon of spectral mimicry. Because of this, the discovery of every new star with a Wolf-Rayet (WR) spectrum requires a special study of its evolutionary status before it can be included in the list of Galactic WR stars. A couple of years ago, LAMOST J040901.83+323955.6 (hereafter J0409+3239) was selected as a WR star in the LAMOST spectroscopic data base by machine-learning methods. In this work, we investigate its evolutionary status. After analysing the spatial location of J0409+3239 in the Galaxy and its position in the colour-magnitude diagram, we conclude that J0409+3239 is instead a low-mass object displayng the WR phenomenon. Its luminosity is L-*=1000 L circle dot and its effective temperature is T-eff = 40 000 K. Using new and archival photometric data, we detected irregular variability on time-scales from hours to tens of days with an amplitude of up to similar to 0.2 mag. A comparison of the spectrum obtained in 2022 with that from 2014 also shows evidence of spectral variability. The absence of a clearly detected circumstellar nebula prevents the classification of J0409+3239 as [WR], namely as the central star of a planetary nebula (CSPN). However, the position of J0409+3239 on the Hertzsprung-Russell diagram suggests that this object is a low-mass star caught in a rare transitional phase to CSPN. Estimation of the J0409+3239 mass based on evolutionary tracks shows that it is less than 0.9 M circle dot, and thus that the age of the Galaxy is barely sufficient for the star to have evolved to its current stage.

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

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2023

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

527

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

10

Strana od-do

11925-11934

Kód UT WoS článku

001142376400019

EID výsledku v databázi Scopus

2-s2.0-85182502726