BU Canis Minoris - the most compact known flat doubly eclipsing quadruple system

Theodor Pribulla; Tamás Borkovits; Rahul Jayaraman; Saul Rappaport; Tibor Mitnyan; Petr Zasche; Richard Komžík; András Pál; Robert Uhlař; Martin Mašek; Zbyněk Henzl; Imre Barna Bíró; István Csányi; Remko Stuik; Martti H. Kristiansen; Hans M. Schwengeler; Robert Gagliano; Thomas L. Jacobs; Mark Omohundro; Veselin Kostov; Brian P. Powell; Ivan A. Terentev; Andrew Vanderburg; Daryll Lacourse; Joseph E. Rodriguez; Gáspár Bakos; Zoltán Csubry; Joel Hartman

doi:10.1093/mnras/stad2015

BU Canis Minoris - the most compact known flat doubly eclipsing quadruple system

Theodor Pribulla, Tamás Borkovits, Rahul Jayaraman, Saul Rappaport, Tibor Mitnyan, Petr Zasche, Richard Komžík, András Pál, Robert Uhlař, Martin Mašek, Zbyněk Henzl, Imre Barna Bíró, István Csányi, Remko Stuik, Martti H. Kristiansen, Hans M. Schwengeler, Robert Gagliano, Thomas L. Jacobs, Mark Omohundro, Veselin KostovBrian P. Powell, Ivan A. Terentev, Andrew Vanderburg, Daryll Lacourse, Joseph E. Rodriguez, Gáspár Bakos, Zoltán Csubry, Joel Hartman

Astrophysical Sciences

Princeton University

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

Abstract

We have found that the 2+2 quadruple star system BU CMi is currently the most compact quadruple system known, with an extremely short outer period of only 121 d. The previous record holder was TIC 219006972 (Kostov et al.), with a period of 168 d. The quadruple nature of BU CMi was established by Volkov, Kravtsova & Chochol, but they misidentified the outer period as 6.6 yr. BU CMi contains two eclipsing binaries (EBs), each with a period near 3 d, and a substantial eccentricity of ≈0.22. All four stars are within ∼0.1 M of 2.4 M. Both binaries exhibit dynamically driven apsidal motion with fairly short apsidal periods of ≈30 yr, due to the short outer orbital period. The outer period of 121 d is found both from the dynamical perturbations, with this period imprinted on the eclipse timing variations curve of each EB by the other binary, and by modelling the complex line profiles in a collection of spectra. We find that the three orbital planes are all mutually aligned to within 1 deg, but the overall system has an inclination angle near 83.5°. We utilize a complex spectro-photodynamical analysis to compute and tabulate all the interesting stellar and orbital parameters of the system. Finally, we also find an unexpected dynamical perturbation on a time-scale of several years whose origin we explore. This latter effect was misinterpreted by Volkov et al. and led them to conclude that the outer period was 6.6 yr rather than the 121 d that we establish here.

Original language	American English
Pages (from-to)	4220-4238
Number of pages	19
Journal	Monthly Notices of the Royal Astronomical Society
Volume	524
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stad2015
State	Published - Sep 1 2023

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Keywords

binaries: eclipsing
binaries: spectroscopic
stars: individual: BU CMi

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10.1093/mnras/stad2015

Cite this

Pribulla, T., Borkovits, T., Jayaraman, R., Rappaport, S., Mitnyan, T., Zasche, P., Komžík, R., Pál, A., Uhlař, R., Mašek, M., Henzl, Z., Bíró, I. B., Csányi, I., Stuik, R., Kristiansen, M. H., Schwengeler, H. M., Gagliano, R., Jacobs, T. L., Omohundro, M., ... Hartman, J. (2023). BU Canis Minoris - the most compact known flat doubly eclipsing quadruple system. Monthly Notices of the Royal Astronomical Society, 524(3), 4220-4238. https://doi.org/10.1093/mnras/stad2015

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title = "BU Canis Minoris - the most compact known flat doubly eclipsing quadruple system",

abstract = "We have found that the 2+2 quadruple star system BU CMi is currently the most compact quadruple system known, with an extremely short outer period of only 121 d. The previous record holder was TIC 219006972 (Kostov et al.), with a period of 168 d. The quadruple nature of BU CMi was established by Volkov, Kravtsova & Chochol, but they misidentified the outer period as 6.6 yr. BU CMi contains two eclipsing binaries (EBs), each with a period near 3 d, and a substantial eccentricity of ≈0.22. All four stars are within ∼0.1 M of 2.4 M. Both binaries exhibit dynamically driven apsidal motion with fairly short apsidal periods of ≈30 yr, due to the short outer orbital period. The outer period of 121 d is found both from the dynamical perturbations, with this period imprinted on the eclipse timing variations curve of each EB by the other binary, and by modelling the complex line profiles in a collection of spectra. We find that the three orbital planes are all mutually aligned to within 1 deg, but the overall system has an inclination angle near 83.5°. We utilize a complex spectro-photodynamical analysis to compute and tabulate all the interesting stellar and orbital parameters of the system. Finally, we also find an unexpected dynamical perturbation on a time-scale of several years whose origin we explore. This latter effect was misinterpreted by Volkov et al. and led them to conclude that the outer period was 6.6 yr rather than the 121 d that we establish here.",

keywords = "binaries: eclipsing, binaries: spectroscopic, stars: individual: BU CMi",

author = "Theodor Pribulla and Tam{\'a}s Borkovits and Rahul Jayaraman and Saul Rappaport and Tibor Mitnyan and Petr Zasche and Richard Kom{\v z}{\'i}k and Andr{\'a}s P{\'a}l and Robert Uhla{\v r} and Martin Ma{\v s}ek and Zbyn{\v e}k Henzl and B{\'i}r{\'o}, {Imre Barna} and Istv{\'a}n Cs{\'a}nyi and Remko Stuik and Kristiansen, {Martti H.} and Schwengeler, {Hans M.} and Robert Gagliano and Jacobs, {Thomas L.} and Mark Omohundro and Veselin Kostov and Powell, {Brian P.} and Terentev, {Ivan A.} and Andrew Vanderburg and Daryll Lacourse and Rodriguez, {Joseph E.} and G{\'a}sp{\'a}r Bakos and Zolt{\'a}n Csubry and Joel Hartman",

note = "Publisher Copyright: {\textcopyright} 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2023",

month = sep,

day = "1",

doi = "10.1093/mnras/stad2015",

language = "American English",

volume = "524",

pages = "4220--4238",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

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Pribulla, T, Borkovits, T, Jayaraman, R, Rappaport, S, Mitnyan, T, Zasche, P, Komžík, R, Pál, A, Uhlař, R, Mašek, M, Henzl, Z, Bíró, IB, Csányi, I, Stuik, R, Kristiansen, MH, Schwengeler, HM, Gagliano, R, Jacobs, TL, Omohundro, M, Kostov, V, Powell, BP, Terentev, IA, Vanderburg, A, Lacourse, D, Rodriguez, JE, Bakos, G, Csubry, Z & Hartman, J 2023, 'BU Canis Minoris - the most compact known flat doubly eclipsing quadruple system', Monthly Notices of the Royal Astronomical Society, vol. 524, no. 3, pp. 4220-4238. https://doi.org/10.1093/mnras/stad2015

TY - JOUR

T1 - BU Canis Minoris - the most compact known flat doubly eclipsing quadruple system

AU - Pribulla, Theodor

AU - Borkovits, Tamás

AU - Jayaraman, Rahul

AU - Rappaport, Saul

AU - Mitnyan, Tibor

AU - Zasche, Petr

AU - Komžík, Richard

AU - Pál, András

AU - Uhlař, Robert

AU - Mašek, Martin

AU - Henzl, Zbyněk

AU - Bíró, Imre Barna

AU - Csányi, István

AU - Stuik, Remko

AU - Kristiansen, Martti H.

AU - Schwengeler, Hans M.

AU - Gagliano, Robert

AU - Jacobs, Thomas L.

AU - Omohundro, Mark

AU - Kostov, Veselin

AU - Powell, Brian P.

AU - Terentev, Ivan A.

AU - Vanderburg, Andrew

AU - Lacourse, Daryll

AU - Rodriguez, Joseph E.

AU - Bakos, Gáspár

AU - Csubry, Zoltán

AU - Hartman, Joel

PY - 2023/9/1

Y1 - 2023/9/1

N2 - We have found that the 2+2 quadruple star system BU CMi is currently the most compact quadruple system known, with an extremely short outer period of only 121 d. The previous record holder was TIC 219006972 (Kostov et al.), with a period of 168 d. The quadruple nature of BU CMi was established by Volkov, Kravtsova & Chochol, but they misidentified the outer period as 6.6 yr. BU CMi contains two eclipsing binaries (EBs), each with a period near 3 d, and a substantial eccentricity of ≈0.22. All four stars are within ∼0.1 M of 2.4 M. Both binaries exhibit dynamically driven apsidal motion with fairly short apsidal periods of ≈30 yr, due to the short outer orbital period. The outer period of 121 d is found both from the dynamical perturbations, with this period imprinted on the eclipse timing variations curve of each EB by the other binary, and by modelling the complex line profiles in a collection of spectra. We find that the three orbital planes are all mutually aligned to within 1 deg, but the overall system has an inclination angle near 83.5°. We utilize a complex spectro-photodynamical analysis to compute and tabulate all the interesting stellar and orbital parameters of the system. Finally, we also find an unexpected dynamical perturbation on a time-scale of several years whose origin we explore. This latter effect was misinterpreted by Volkov et al. and led them to conclude that the outer period was 6.6 yr rather than the 121 d that we establish here.

AB - We have found that the 2+2 quadruple star system BU CMi is currently the most compact quadruple system known, with an extremely short outer period of only 121 d. The previous record holder was TIC 219006972 (Kostov et al.), with a period of 168 d. The quadruple nature of BU CMi was established by Volkov, Kravtsova & Chochol, but they misidentified the outer period as 6.6 yr. BU CMi contains two eclipsing binaries (EBs), each with a period near 3 d, and a substantial eccentricity of ≈0.22. All four stars are within ∼0.1 M of 2.4 M. Both binaries exhibit dynamically driven apsidal motion with fairly short apsidal periods of ≈30 yr, due to the short outer orbital period. The outer period of 121 d is found both from the dynamical perturbations, with this period imprinted on the eclipse timing variations curve of each EB by the other binary, and by modelling the complex line profiles in a collection of spectra. We find that the three orbital planes are all mutually aligned to within 1 deg, but the overall system has an inclination angle near 83.5°. We utilize a complex spectro-photodynamical analysis to compute and tabulate all the interesting stellar and orbital parameters of the system. Finally, we also find an unexpected dynamical perturbation on a time-scale of several years whose origin we explore. This latter effect was misinterpreted by Volkov et al. and led them to conclude that the outer period was 6.6 yr rather than the 121 d that we establish here.

KW - binaries: eclipsing

KW - binaries: spectroscopic

KW - stars: individual: BU CMi

UR - http://www.scopus.com/inward/record.url?scp=85168139324&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85168139324&partnerID=8YFLogxK

U2 - 10.1093/mnras/stad2015

DO - 10.1093/mnras/stad2015

M3 - Article

SN - 0035-8711

VL - 524

SP - 4220

EP - 4238

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

BU Canis Minoris - the most compact known flat doubly eclipsing quadruple system

Abstract

ASJC Scopus subject areas

Keywords

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