A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass-Radius Relationship for M Dwarfs

Jack B. Lubin; Joseph E. Rodriguez; George Zhou; Kyle E. Conroy; Keivan G. Stassun; Karen Collins; Daniel J. Stevens; Jonathan Labadie-Bartz; Christopher Stockdale; Gordon Myers; Knicole D. Colón; Joao Bento; Petri Kehusmaa; Romina Petrucci; Emiliano Jofré; Samuel N. Quinn; Michael B. Lund; Rudolf B. Kuhn; Robert J. Siverd; Thomas G. Beatty; Caisey Harlingten; Joshua Pepper; B. Scott Gaudi; David James; Eric L.N. Jensen; Daniel Reichart; Lucyna Kedziora-Chudczer; Jeremy Bailey; Graeme Melville

doi:10.3847/1538-4357/aa7947

A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass-Radius Relationship for M Dwarfs

Jack B. Lubin, Joseph E. Rodriguez^*, George Zhou, Kyle E. Conroy, Keivan G. Stassun, Karen Collins, Daniel J. Stevens, Jonathan Labadie-Bartz, Christopher Stockdale, Gordon Myers, Knicole D. Colón, Joao Bento, Petri Kehusmaa, Romina Petrucci, Emiliano Jofré, Samuel N. Quinn, Michael B. Lund, Rudolf B. Kuhn, Robert J. Siverd, Thomas G. BeattyCaisey Harlingten, Joshua Pepper, B. Scott Gaudi, David James, Eric L.N. Jensen, Daniel Reichart, Lucyna Kedziora-Chudczer, Jeremy Bailey, Graeme Melville

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

17 Citations (Scopus)

Abstract

We report the discovery of KELT J041621-620046, a moderately bright (J ∼ 10.2) M-dwarf eclipsing binary system at a distance of 39 ± 3 pc. KELT J041621-620046 was first identified as an eclipsing binary using observations from the Kilodegree Extremely Little Telescope (KELT) survey. The system has a short orbital period of ∼1.11 days and consists of components with M₁ = 0.447^+0.052_-0.047 M_⊙ and M₂ = 0.399^+0.046-0.042 M_⊙ in nearly circular orbits. The radii of the two stars are R₁ = 0.540^+0.034_-0.032 R_⊙ and R₂ = 0.453 &plummn; 0.017 R_⊙. Full system and orbital properties were determined (to ∼10% error) by conducting an EBOP (Eclipsing Binary Orbit Program) global modeling of the high precision photometric and spectroscopic observations obtained by the KELT Follow-up Network. Each star is larger by 17%-28% and cooler by 4%-10% than predicted by standard (non-magnetic) stellar models. Strong Hα emission indicates chromospheric activity in both stars. The observed radii and temperature discrepancies for both components are more consistent with those predicted by empirical relations that account for convective suppression due to magnetic activity.

Original language	English
Article number	134
Journal	Astrophysical Journal
Volume	844
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/aa7947
Publication status	Published - 1 Aug 2017

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Lubin, J. B., Rodriguez, J. E., Zhou, G., Conroy, K. E., Stassun, K. G., Collins, K., Stevens, D. J., Labadie-Bartz, J., Stockdale, C., Myers, G., Colón, K. D., Bento, J., Kehusmaa, P., Petrucci, R., Jofré, E., Quinn, S. N., Lund, M. B., Kuhn, R. B., Siverd, R. J., ... Melville, G. (2017). A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass-Radius Relationship for M Dwarfs. Astrophysical Journal, 844(2), Article 134. https://doi.org/10.3847/1538-4357/aa7947

@article{aee250ee371f47e594c2fb38fd7899a4,

title = "A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass-Radius Relationship for M Dwarfs",

abstract = "We report the discovery of KELT J041621-620046, a moderately bright (J ∼ 10.2) M-dwarf eclipsing binary system at a distance of 39 ± 3 pc. KELT J041621-620046 was first identified as an eclipsing binary using observations from the Kilodegree Extremely Little Telescope (KELT) survey. The system has a short orbital period of ∼1.11 days and consists of components with M1 = 0.447+0.052-0.047 M⊙ and M2 = 0.399+0.046-0.042 M⊙ in nearly circular orbits. The radii of the two stars are R1 = 0.540+0.034-0.032 R⊙ and R2 = 0.453 &plummn; 0.017 R⊙. Full system and orbital properties were determined (to ∼10% error) by conducting an EBOP (Eclipsing Binary Orbit Program) global modeling of the high precision photometric and spectroscopic observations obtained by the KELT Follow-up Network. Each star is larger by 17%-28% and cooler by 4%-10% than predicted by standard (non-magnetic) stellar models. Strong Hα emission indicates chromospheric activity in both stars. The observed radii and temperature discrepancies for both components are more consistent with those predicted by empirical relations that account for convective suppression due to magnetic activity.",

keywords = "binaries: eclipsing, binaries: general, stars: low-mass",

author = "Lubin, {Jack B.} and Rodriguez, {Joseph E.} and George Zhou and Conroy, {Kyle E.} and Stassun, {Keivan G.} and Karen Collins and Stevens, {Daniel J.} and Jonathan Labadie-Bartz and Christopher Stockdale and Gordon Myers and Col{\'o}n, {Knicole D.} and Joao Bento and Petri Kehusmaa and Romina Petrucci and Emiliano Jofr{\'e} and Quinn, {Samuel N.} and Lund, {Michael B.} and Kuhn, {Rudolf B.} and Siverd, {Robert J.} and Beatty, {Thomas G.} and Caisey Harlingten and Joshua Pepper and Gaudi, {B. Scott} and David James and Jensen, {Eric L.N.} and Daniel Reichart and Lucyna Kedziora-Chudczer and Jeremy Bailey and Graeme Melville",

year = "2017",

month = aug,

day = "1",

doi = "10.3847/1538-4357/aa7947",

language = "English",

volume = "844",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Lubin, JB, Rodriguez, JE, Zhou, G, Conroy, KE, Stassun, KG, Collins, K, Stevens, DJ, Labadie-Bartz, J, Stockdale, C, Myers, G, Colón, KD, Bento, J, Kehusmaa, P, Petrucci, R, Jofré, E, Quinn, SN, Lund, MB, Kuhn, RB, Siverd, RJ, Beatty, TG, Harlingten, C, Pepper, J, Gaudi, BS, James, D, Jensen, ELN, Reichart, D, Kedziora-Chudczer, L, Bailey, J & Melville, G 2017, 'A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass-Radius Relationship for M Dwarfs', Astrophysical Journal, vol. 844, no. 2, 134. https://doi.org/10.3847/1538-4357/aa7947

TY - JOUR

T1 - A Bright Short Period M-M Eclipsing Binary from the KELT Survey

T2 - Magnetic Activity and the Mass-Radius Relationship for M Dwarfs

AU - Lubin, Jack B.

AU - Rodriguez, Joseph E.

AU - Zhou, George

AU - Conroy, Kyle E.

AU - Stassun, Keivan G.

AU - Collins, Karen

AU - Stevens, Daniel J.

AU - Labadie-Bartz, Jonathan

AU - Stockdale, Christopher

AU - Myers, Gordon

AU - Colón, Knicole D.

AU - Bento, Joao

AU - Kehusmaa, Petri

AU - Petrucci, Romina

AU - Jofré, Emiliano

AU - Quinn, Samuel N.

AU - Lund, Michael B.

AU - Kuhn, Rudolf B.

AU - Siverd, Robert J.

AU - Beatty, Thomas G.

AU - Harlingten, Caisey

AU - Pepper, Joshua

AU - Gaudi, B. Scott

AU - James, David

AU - Jensen, Eric L.N.

AU - Reichart, Daniel

AU - Kedziora-Chudczer, Lucyna

AU - Bailey, Jeremy

AU - Melville, Graeme

PY - 2017/8/1

Y1 - 2017/8/1

N2 - We report the discovery of KELT J041621-620046, a moderately bright (J ∼ 10.2) M-dwarf eclipsing binary system at a distance of 39 ± 3 pc. KELT J041621-620046 was first identified as an eclipsing binary using observations from the Kilodegree Extremely Little Telescope (KELT) survey. The system has a short orbital period of ∼1.11 days and consists of components with M1 = 0.447+0.052-0.047 M⊙ and M2 = 0.399+0.046-0.042 M⊙ in nearly circular orbits. The radii of the two stars are R1 = 0.540+0.034-0.032 R⊙ and R2 = 0.453 &plummn; 0.017 R⊙. Full system and orbital properties were determined (to ∼10% error) by conducting an EBOP (Eclipsing Binary Orbit Program) global modeling of the high precision photometric and spectroscopic observations obtained by the KELT Follow-up Network. Each star is larger by 17%-28% and cooler by 4%-10% than predicted by standard (non-magnetic) stellar models. Strong Hα emission indicates chromospheric activity in both stars. The observed radii and temperature discrepancies for both components are more consistent with those predicted by empirical relations that account for convective suppression due to magnetic activity.

AB - We report the discovery of KELT J041621-620046, a moderately bright (J ∼ 10.2) M-dwarf eclipsing binary system at a distance of 39 ± 3 pc. KELT J041621-620046 was first identified as an eclipsing binary using observations from the Kilodegree Extremely Little Telescope (KELT) survey. The system has a short orbital period of ∼1.11 days and consists of components with M1 = 0.447+0.052-0.047 M⊙ and M2 = 0.399+0.046-0.042 M⊙ in nearly circular orbits. The radii of the two stars are R1 = 0.540+0.034-0.032 R⊙ and R2 = 0.453 &plummn; 0.017 R⊙. Full system and orbital properties were determined (to ∼10% error) by conducting an EBOP (Eclipsing Binary Orbit Program) global modeling of the high precision photometric and spectroscopic observations obtained by the KELT Follow-up Network. Each star is larger by 17%-28% and cooler by 4%-10% than predicted by standard (non-magnetic) stellar models. Strong Hα emission indicates chromospheric activity in both stars. The observed radii and temperature discrepancies for both components are more consistent with those predicted by empirical relations that account for convective suppression due to magnetic activity.

KW - binaries: eclipsing

KW - binaries: general

KW - stars: low-mass

UR - http://www.scopus.com/inward/record.url?scp=85088877892&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/aa7947

DO - 10.3847/1538-4357/aa7947

M3 - Article

SN - 0004-637X

VL - 844

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 134

ER -

A Bright Short Period M-M Eclipsing Binary from the KELT Survey: Magnetic Activity and the Mass-Radius Relationship for M Dwarfs

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