The EBLM project

II. A very hot, low-mass M dwarf in an eccentric and long-period, eclipsing binary system from the SuperWASP survey

Y. Gómez Maqueo Chew, J. C. Morales, F. Faedi, E. García-Melendo, L. Hebb, F. Rodler, R. Deshpande, Suvrath Mahadevan, J. McCormac, R. Barnes, A. H.M.J. Triaud, M. Lopez-Morales, I. Skillen, A. Collier Cameron, M. D. Joner, C. D. Laney, D. C. Stephens, K. G. Stassun, P. A. Cargile, P. Montañés-Rodríguez

Research output: Contribution to journalArticle

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Abstract

In this paper, we derive the fundamental properties of 1SWASPJ011351.29+314909.7 (J0113+31), a metal-poor (-0.40 ± 0.04 dex), eclipsing binary in an eccentric orbit (∼0.3) with an orbital period of ∼14.277 d. Eclipsing M dwarfs that orbit solar-type stars (EBLMs), like J0113+31, have been identified from their light curves and follow-up spectroscopy in the course of the WASP transiting planet search. We present the analysis of the first binary of the EBLM sample for which masses, radii and temperatures of both components are derived, and thus, define here the methodology. The primary component with a mass of 0.945? ±? 0.045 M? has a large radius (1.378±0.058 R?) indicating that the system is quite old, ∼9.5 Gyr. The M-dwarf secondary mass of 0.186? ±? 0.010 M? and radius of 0.209? ±? 0.011 R? are fully consistent with stellar evolutionary models. However, from the near-infrared secondary eclipse light curve, the M dwarf is found to have an effective temperature of 3922? ±? 42 K, which is ∼600 K hotter than predicted by theoretical models. We discuss different scenarios to explain this temperature discrepancy. The case of J0113+31 for which we can measure mass, radius, temperature, and metallicity highlights the importance of deriving mass, radius, and temperature as a function of metallicity for M dwarfs to better understand the lowest mass stars. The EBLM Project will define the relationship between mass, radius, temperature, and metallicityfor M dwarfs providing important empirical constraints at the bottom of the main sequence.

Original languageEnglish (US)
Article numberA50
JournalAstronomy and Astrophysics
Volume572
DOIs
StatePublished - Dec 1 2014

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eccentrics
radii
temperature
light curve
metallicity
solar orbits
stars
eccentric orbits
stellar models
eclipses
project
planets
near infrared
planet
spectroscopy
methodology
orbitals
metal
metals

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Gómez Maqueo Chew, Y., Morales, J. C., Faedi, F., García-Melendo, E., Hebb, L., Rodler, F., ... Montañés-Rodríguez, P. (2014). The EBLM project: II. A very hot, low-mass M dwarf in an eccentric and long-period, eclipsing binary system from the SuperWASP survey. Astronomy and Astrophysics, 572, [A50]. https://doi.org/10.1051/0004-6361/201424265
Gómez Maqueo Chew, Y. ; Morales, J. C. ; Faedi, F. ; García-Melendo, E. ; Hebb, L. ; Rodler, F. ; Deshpande, R. ; Mahadevan, Suvrath ; McCormac, J. ; Barnes, R. ; Triaud, A. H.M.J. ; Lopez-Morales, M. ; Skillen, I. ; Collier Cameron, A. ; Joner, M. D. ; Laney, C. D. ; Stephens, D. C. ; Stassun, K. G. ; Cargile, P. A. ; Montañés-Rodríguez, P. / The EBLM project : II. A very hot, low-mass M dwarf in an eccentric and long-period, eclipsing binary system from the SuperWASP survey. In: Astronomy and Astrophysics. 2014 ; Vol. 572.
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title = "The EBLM project: II. A very hot, low-mass M dwarf in an eccentric and long-period, eclipsing binary system from the SuperWASP survey",
abstract = "In this paper, we derive the fundamental properties of 1SWASPJ011351.29+314909.7 (J0113+31), a metal-poor (-0.40 ± 0.04 dex), eclipsing binary in an eccentric orbit (∼0.3) with an orbital period of ∼14.277 d. Eclipsing M dwarfs that orbit solar-type stars (EBLMs), like J0113+31, have been identified from their light curves and follow-up spectroscopy in the course of the WASP transiting planet search. We present the analysis of the first binary of the EBLM sample for which masses, radii and temperatures of both components are derived, and thus, define here the methodology. The primary component with a mass of 0.945? ±? 0.045 M? has a large radius (1.378±0.058 R?) indicating that the system is quite old, ∼9.5 Gyr. The M-dwarf secondary mass of 0.186? ±? 0.010 M? and radius of 0.209? ±? 0.011 R? are fully consistent with stellar evolutionary models. However, from the near-infrared secondary eclipse light curve, the M dwarf is found to have an effective temperature of 3922? ±? 42 K, which is ∼600 K hotter than predicted by theoretical models. We discuss different scenarios to explain this temperature discrepancy. The case of J0113+31 for which we can measure mass, radius, temperature, and metallicity highlights the importance of deriving mass, radius, and temperature as a function of metallicity for M dwarfs to better understand the lowest mass stars. The EBLM Project will define the relationship between mass, radius, temperature, and metallicityfor M dwarfs providing important empirical constraints at the bottom of the main sequence.",
author = "{G{\'o}mez Maqueo Chew}, Y. and Morales, {J. C.} and F. Faedi and E. Garc{\'i}a-Melendo and L. Hebb and F. Rodler and R. Deshpande and Suvrath Mahadevan and J. McCormac and R. Barnes and Triaud, {A. H.M.J.} and M. Lopez-Morales and I. Skillen and {Collier Cameron}, A. and Joner, {M. D.} and Laney, {C. D.} and Stephens, {D. C.} and Stassun, {K. G.} and Cargile, {P. A.} and P. Monta{\~n}{\'e}s-Rodr{\'i}guez",
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Gómez Maqueo Chew, Y, Morales, JC, Faedi, F, García-Melendo, E, Hebb, L, Rodler, F, Deshpande, R, Mahadevan, S, McCormac, J, Barnes, R, Triaud, AHMJ, Lopez-Morales, M, Skillen, I, Collier Cameron, A, Joner, MD, Laney, CD, Stephens, DC, Stassun, KG, Cargile, PA & Montañés-Rodríguez, P 2014, 'The EBLM project: II. A very hot, low-mass M dwarf in an eccentric and long-period, eclipsing binary system from the SuperWASP survey', Astronomy and Astrophysics, vol. 572, A50. https://doi.org/10.1051/0004-6361/201424265

The EBLM project : II. A very hot, low-mass M dwarf in an eccentric and long-period, eclipsing binary system from the SuperWASP survey. / Gómez Maqueo Chew, Y.; Morales, J. C.; Faedi, F.; García-Melendo, E.; Hebb, L.; Rodler, F.; Deshpande, R.; Mahadevan, Suvrath; McCormac, J.; Barnes, R.; Triaud, A. H.M.J.; Lopez-Morales, M.; Skillen, I.; Collier Cameron, A.; Joner, M. D.; Laney, C. D.; Stephens, D. C.; Stassun, K. G.; Cargile, P. A.; Montañés-Rodríguez, P.

In: Astronomy and Astrophysics, Vol. 572, A50, 01.12.2014.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The EBLM project

T2 - II. A very hot, low-mass M dwarf in an eccentric and long-period, eclipsing binary system from the SuperWASP survey

AU - Gómez Maqueo Chew, Y.

AU - Morales, J. C.

AU - Faedi, F.

AU - García-Melendo, E.

AU - Hebb, L.

AU - Rodler, F.

AU - Deshpande, R.

AU - Mahadevan, Suvrath

AU - McCormac, J.

AU - Barnes, R.

AU - Triaud, A. H.M.J.

AU - Lopez-Morales, M.

AU - Skillen, I.

AU - Collier Cameron, A.

AU - Joner, M. D.

AU - Laney, C. D.

AU - Stephens, D. C.

AU - Stassun, K. G.

AU - Cargile, P. A.

AU - Montañés-Rodríguez, P.

PY - 2014/12/1

Y1 - 2014/12/1

N2 - In this paper, we derive the fundamental properties of 1SWASPJ011351.29+314909.7 (J0113+31), a metal-poor (-0.40 ± 0.04 dex), eclipsing binary in an eccentric orbit (∼0.3) with an orbital period of ∼14.277 d. Eclipsing M dwarfs that orbit solar-type stars (EBLMs), like J0113+31, have been identified from their light curves and follow-up spectroscopy in the course of the WASP transiting planet search. We present the analysis of the first binary of the EBLM sample for which masses, radii and temperatures of both components are derived, and thus, define here the methodology. The primary component with a mass of 0.945? ±? 0.045 M? has a large radius (1.378±0.058 R?) indicating that the system is quite old, ∼9.5 Gyr. The M-dwarf secondary mass of 0.186? ±? 0.010 M? and radius of 0.209? ±? 0.011 R? are fully consistent with stellar evolutionary models. However, from the near-infrared secondary eclipse light curve, the M dwarf is found to have an effective temperature of 3922? ±? 42 K, which is ∼600 K hotter than predicted by theoretical models. We discuss different scenarios to explain this temperature discrepancy. The case of J0113+31 for which we can measure mass, radius, temperature, and metallicity highlights the importance of deriving mass, radius, and temperature as a function of metallicity for M dwarfs to better understand the lowest mass stars. The EBLM Project will define the relationship between mass, radius, temperature, and metallicityfor M dwarfs providing important empirical constraints at the bottom of the main sequence.

AB - In this paper, we derive the fundamental properties of 1SWASPJ011351.29+314909.7 (J0113+31), a metal-poor (-0.40 ± 0.04 dex), eclipsing binary in an eccentric orbit (∼0.3) with an orbital period of ∼14.277 d. Eclipsing M dwarfs that orbit solar-type stars (EBLMs), like J0113+31, have been identified from their light curves and follow-up spectroscopy in the course of the WASP transiting planet search. We present the analysis of the first binary of the EBLM sample for which masses, radii and temperatures of both components are derived, and thus, define here the methodology. The primary component with a mass of 0.945? ±? 0.045 M? has a large radius (1.378±0.058 R?) indicating that the system is quite old, ∼9.5 Gyr. The M-dwarf secondary mass of 0.186? ±? 0.010 M? and radius of 0.209? ±? 0.011 R? are fully consistent with stellar evolutionary models. However, from the near-infrared secondary eclipse light curve, the M dwarf is found to have an effective temperature of 3922? ±? 42 K, which is ∼600 K hotter than predicted by theoretical models. We discuss different scenarios to explain this temperature discrepancy. The case of J0113+31 for which we can measure mass, radius, temperature, and metallicity highlights the importance of deriving mass, radius, and temperature as a function of metallicity for M dwarfs to better understand the lowest mass stars. The EBLM Project will define the relationship between mass, radius, temperature, and metallicityfor M dwarfs providing important empirical constraints at the bottom of the main sequence.

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U2 - 10.1051/0004-6361/201424265

DO - 10.1051/0004-6361/201424265

M3 - Article

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JO - Astronomy and Astrophysics

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