The double low-mass white dwarf eclipsing binary system J2102-4145 and its possible evolution

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00586941" target="_blank" >RIV/67985815:_____/24:00586941 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0354889" target="_blank" >https://hdl.handle.net/11104/0354889</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202348564" target="_blank" >10.1051/0004-6361/202348564</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The double low-mass white dwarf eclipsing binary system J2102-4145 and its possible evolution

Popis výsledku v původním jazyce

In recent years, about 150 low-mass white dwarfs (WDs), typically with masses below 0.4 M-circle dot, have been discovered. The majority of these low-mass WDs are observed in binary systems as they cannot be formed through single-star evolution within Hubble time. In this work, we present a comprehensive analysis of the double low-mass WD eclipsing binary system J2102 4145. Our investigation encompasses an extensive observational campaign, resulting in the acquisition of approximately 28 h of high-speed photometric data across multiple nights using NTT /ULTRACAM, SOAR /Goodman, and SMARTS-1m telescopes. These observations have provided critical insights into the orbital characteristics of this system, including parameters such as inclination and orbital period. To disentangle the binary components of J2102 4145, we employed the XTgrid spectral fitting method with GMOS /Gemini-South and X-shooter data. Additionally, we used the PHOEBE package for light curve analysis on NTT/ULTRACAM high-speed time-series photometry data to constrain the binary star properties. Our analysis unveils remarkable similarities between the two components of this binary system. For the primary star, we determine T-eff,T-1 = 13 688(-72)(+65) K, log g(1) = 7.36 +/- 0.01, R-1 = 0.0211 +/- 0.0002 R-circle dot, and M-1 = 0.375 +/- 0.003 M-circle dot, while, the secondary star is characterised by T-eff,T-2 = 12 952 +/- 53 66 K, log g(2) = 7.32 +/- 0.01, R-2 = 0.0203 +/- 0.0002 0.0003 R-circle dot, and M-2 = 0.314 +/- 0.003 M-circle dot. Furthermore, we found a notable discrepancy between T-eff and R of the less massive WD, compared to evolutionary sequences for WDs from the literature, which has significant implications for our understanding of WD evolution. We discuss a potential formation scenario for this system which might explain this discrepancy and explore its future evolution. We predict that this system will merge in similar to 800 Myr, evolving into a helium-rich hot subdwarf star and later into a hybrid He/CO WD.

Název v anglickém jazyce

The double low-mass white dwarf eclipsing binary system J2102-4145 and its possible evolution

Popis výsledku anglicky

In recent years, about 150 low-mass white dwarfs (WDs), typically with masses below 0.4 M-circle dot, have been discovered. The majority of these low-mass WDs are observed in binary systems as they cannot be formed through single-star evolution within Hubble time. In this work, we present a comprehensive analysis of the double low-mass WD eclipsing binary system J2102 4145. Our investigation encompasses an extensive observational campaign, resulting in the acquisition of approximately 28 h of high-speed photometric data across multiple nights using NTT /ULTRACAM, SOAR /Goodman, and SMARTS-1m telescopes. These observations have provided critical insights into the orbital characteristics of this system, including parameters such as inclination and orbital period. To disentangle the binary components of J2102 4145, we employed the XTgrid spectral fitting method with GMOS /Gemini-South and X-shooter data. Additionally, we used the PHOEBE package for light curve analysis on NTT/ULTRACAM high-speed time-series photometry data to constrain the binary star properties. Our analysis unveils remarkable similarities between the two components of this binary system. For the primary star, we determine T-eff,T-1 = 13 688(-72)(+65) K, log g(1) = 7.36 +/- 0.01, R-1 = 0.0211 +/- 0.0002 R-circle dot, and M-1 = 0.375 +/- 0.003 M-circle dot, while, the secondary star is characterised by T-eff,T-2 = 12 952 +/- 53 66 K, log g(2) = 7.32 +/- 0.01, R-2 = 0.0203 +/- 0.0002 0.0003 R-circle dot, and M-2 = 0.314 +/- 0.003 M-circle dot. Furthermore, we found a notable discrepancy between T-eff and R of the less massive WD, compared to evolutionary sequences for WDs from the literature, which has significant implications for our understanding of WD evolution. We discuss a potential formation scenario for this system which might explain this discrepancy and explore its future evolution. We predict that this system will merge in similar to 800 Myr, evolving into a helium-rich hot subdwarf star and later into a hybrid He/CO WD.

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/GA22-34467S" target="_blank" >GA22-34467S: Interakce dvojhvězd na větvi červených obrů: horcí podtrpaslíci jako testovací případ.</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2024

Kód důvěrnosti údajů

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

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

685

Číslo periodika v rámci svazku

May

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

17

Strana od-do

A9

Kód UT WoS článku

001231008100026

EID výsledku v databázi Scopus

2-s2.0-85192486993