Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown
dwarf as possible evidence of deuterium burning at old stellar
ages

J 2024

Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages

SUBJAK, Jan; David W LATHAM; Samuel N QUINN; Perry BERLIND; Michael L CALKINS et al.

Základní údaje

Originální název

Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages

Autoři

Vydání

Astronomy and Astrophysics, LES ULIS CEDEX A, EDP SCIENCES S A, 2024, 0004-6361

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Odkazy

URL

Impakt faktor

Impact factor: 5.800

Označené pro přenos do RIV

Ano

Kód RIV

RIV/00216224:14310/24:00137211

Organizační jednotka

Přírodovědecká fakulta

Klíčová slova anglicky

techniques: photometric; techniques: radial velocities; techniques: spectroscopic; planets and satellites: gaseous planets; brown dwarfs

Štítky

14312040, rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 14. 3. 2025 12:06, Mgr. Marie Novosadová Šípková, DiS.

Anotace

V originále

The present study confirms BD-14 3065b as a transiting planet-brown dwarf in a triple-star system, with a mass near the deuterium-burning boundary. BD-14 3065b has the largest radius observed within the sample of giant planets and brown dwarfs around post-main sequence stars. Its orbital period is 4.3 days and it transits a subgiant F-type star with a mass of M-* = 1.41 +/- 0.05 M-circle dot, a radius of R-* = 2.35 +/- 0.08 R-circle dot, an effective temperature of T-eff = 6935 +/- 90 K, and a metallicity of -0.34 +/- 0.05 dex. By combining TESS photometry with high-resolution spectra acquired with the TRES and Pucheros+ spectrographs, we measured a mass of M-p = 12.37 +/- 0.92 M-Jup and a radius of R-p = 1.926 +/- 0.094 R-Jup. Our discussion of potential processes that could be responsible for the inflated radius led us to conclude that deuterium burning is a plausible explanation for the heating taking place in BD-14 3065b's interior. Detections of the secondary eclipse with TESS photometry enabled a precise determination of the eccentricity, e(p) = 0.066 +/- 0.011, and reveal that BD-14 3065b has a brightness temperature of 3520 +/- 130 K. With its unique characteristics, BD-14 3065b presents an excellent opportunity to study its atmosphere via thermal emission spectroscopy.

Citovat

SUBJAK, Jan; David W LATHAM; Samuel N QUINN; Perry BERLIND; Michael L CALKINS; Gilbert A ESQUERDO; Rafael BRAHM; Jose A CABALLERO; Karen A COLLINS; Eike GUENTHER; Jan JANÍK; Petr KABÁTH; Richard P SCHWARZ; Thiam-Guan TAN; Leonardo VANZI; Roberto ZAMBELLI; Carl ZIEGLER; Jon M JENKINS; Ismael MIRELES; Sara SEAGER; Avi SHPORER; Stephanie STRIEGEL a Joshua N WINN. Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages. Astronomy and Astrophysics. LES ULIS CEDEX A: EDP SCIENCES S A, 2024, roč. 688, August, s. 1-23. ISSN 0004-6361. Dostupné z: https://doi.org/10.1051/0004-6361/202349028.

@article{2437202,
   author = {Subjak, Jan and Latham, David W and Quinn, Samuel N and Berlind, Perry and Calkins, Michael L and Esquerdo, Gilbert A and Brahm, Rafael and Caballero, Jose A and Collins, Karen A and Guenther, Eike and Janík, Jan and Kabáth, Petr and Schwarz, Richard P and Tan, ThiamandGuan and Vanzi, Leonardo and Zambelli, Roberto and Ziegler, Carl and Jenkins, Jon M and Mireles, Ismael and Seager, Sara and Shporer, Avi and Striegel, Stephanie and Winn, Joshua N},
   article_location = {LES ULIS CEDEX A},
   article_number = {August},
   doi = {https://doi.org/10.1051/0004-6361/202349028},
   keywords = {techniques: photometric; techniques: radial velocities; techniques: spectroscopic; planets and satellites: gaseous planets; brown dwarfs},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages},
   url = {https://www.aanda.org/articles/aa/pdf/2024/08/aa49028-23.pdf},
   volume = {688},
   year = {2024}
}

TY  - JOUR
ID  - 2437202
AU  - Subjak, Jan - Latham, David W - Quinn, Samuel N - Berlind, Perry - Calkins, Michael L - Esquerdo, Gilbert A - Brahm, Rafael - Caballero, Jose A - Collins, Karen A - Guenther, Eike - Janík, Jan - Kabáth, Petr - Schwarz, Richard P - Tan, Thiam-Guan - Vanzi, Leonardo - Zambelli, Roberto - Ziegler, Carl - Jenkins, Jon M - Mireles, Ismael - Seager, Sara - Shporer, Avi - Striegel, Stephanie - Winn, Joshua N
PY  - 2024
TI  - Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages
JF  - Astronomy and Astrophysics
VL  - 688
IS  - August
SP  - 1-23
EP  - 1-23
PB  - EDP SCIENCES S A
SN  - 00046361
KW  - techniques: photometric
KW  - techniques: radial velocities
KW  - techniques: spectroscopic
KW  - planets and satellites: gaseous planets
KW  - brown dwarfs
UR  - https://www.aanda.org/articles/aa/pdf/2024/08/aa49028-23.pdf
N2  - The present study confirms BD-14 3065b as a transiting planet-brown dwarf in a triple-star system, with a mass near the deuterium-burning boundary. BD-14 3065b has the largest radius observed within the sample of giant planets and brown dwarfs around post-main sequence stars. Its orbital period is 4.3 days and it transits a subgiant F-type star with a mass of M-* = 1.41 +/- 0.05 M-circle dot, a radius of R-* = 2.35 +/- 0.08 R-circle dot, an effective temperature of T-eff = 6935 +/- 90 K, and a metallicity of -0.34 +/- 0.05 dex. By combining TESS photometry with high-resolution spectra acquired with the TRES and Pucheros+ spectrographs, we measured a mass of M-p = 12.37 +/- 0.92 M-Jup and a radius of R-p = 1.926 +/- 0.094 R-Jup. Our discussion of potential processes that could be responsible for the inflated radius led us to conclude that deuterium burning is a plausible explanation for the heating taking place in BD-14 3065b's interior. Detections of the secondary eclipse with TESS photometry enabled a precise determination of the eccentricity, e(p) = 0.066 +/- 0.011, and reveal that BD-14 3065b has a brightness temperature of 3520 +/- 130 K. With its unique characteristics, BD-14 3065b presents an excellent opportunity to study its atmosphere via thermal emission spectroscopy.
ER  -

SUBJAK, Jan; David W LATHAM; Samuel N QUINN; Perry BERLIND; Michael L CALKINS; Gilbert A ESQUERDO; Rafael BRAHM; Jose A CABALLERO; Karen A COLLINS; Eike GUENTHER; Jan JANÍK; Petr KABÁTH; Richard P SCHWARZ; Thiam-Guan TAN; Leonardo VANZI; Roberto ZAMBELLI; Carl ZIEGLER; Jon M JENKINS; Ismael MIRELES; Sara SEAGER; Avi SHPORER; Stephanie STRIEGEL a Joshua N WINN. Evolution of BD-14 3065b (TOI-4987b) from giant planet to brown dwarf as possible evidence of deuterium burning at old stellar ages. \textit{Astronomy and Astrophysics}. LES ULIS CEDEX A: EDP SCIENCES S A, 2024, roč.~688, August, s.~1-23. ISSN~0004-6361. Dostupné z: https://doi.org/10.1051/0004-6361/202349028.

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