Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars

We previously reported a rare class of variable star light curves isolated from a sample of 4.7 million candidate variables from the ATLAS survey. Dubbed “UCBH” light curves, they have broad minima and narrow, symmetrical maxima, with typical periods of 1–10 days and amplitudes of 0.05–0.20 mag. The...
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Autor*in:	A. N. Heinze [verfasserIn] Heather Flewelling [verfasserIn] Mark E. Huber [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Peculiar variable stars Chemically peculiar stars Variable stars Magnetic variable stars Ap stars Silicon stars

Übergeordnetes Werk:	In: The Astronomical Journal - IOP Publishing, 2022, 166(2023), 4, p 169
Übergeordnetes Werk:	volume:166 ; year:2023 ; number:4, p 169

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-3881/acf7c0

Katalog-ID:	DOAJ091857406

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allfields	10.3847/1538-3881/acf7c0 doi (DE-627)DOAJ091857406 (DE-599)DOAJd35c991048f842f4b9844c174c812a97 DE-627 ger DE-627 rakwb eng QB1-991 A. N. Heinze verfasserin aut Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We previously reported a rare class of variable star light curves isolated from a sample of 4.7 million candidate variables from the ATLAS survey. Dubbed “UCBH” light curves, they have broad minima and narrow, symmetrical maxima, with typical periods of 1–10 days and amplitudes of 0.05–0.20 mag. They maintain constant amplitude, shape, and phase coherence over multiple years but do not match any known class of pulsating variables. A localized bright spot near the equator of a rotating star will produce a UCBH-type light curve for most viewing geometries. Most stars that exhibit rotational variability caused primarily by a single bright feature should therefore appear as UCBH stars, although a rotating bright spot is not the only thing that could produce a UCBH-type light curve. We have spectroscopically investigated 14 UCBH stars and found 10 of them to be Ap/Bp stars: A-type or B-type stars with greatly enhanced photospheric abundances of specific heavy elements. Rotationally variable Ap/Bp stars are referred to as α ^2 CVn variables. Most ATLAS UCBH stars are therefore α ^2 CVn stars, although only a minority of α ^2 CVn stars in the literature have UCBH light curves. The fact that α ^2 CVn stars dominate the UCBH class suggests that lone bright spots with sufficient size and contrast develop more readily on Ap/Bp stars than on any other type. The α ^2 CVn UCBH stars may be characterized by a specific magnetic field topology, making them intriguing targets for future Zeeman–Doppler imaging. Peculiar variable stars Chemically peculiar stars Variable stars Magnetic variable stars Ap stars Silicon stars Astronomy Heather Flewelling verfasserin aut Mark E. Huber verfasserin aut In The Astronomical Journal IOP Publishing, 2022 166(2023), 4, p 169 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:166 year:2023 number:4, p 169 https://doi.org/10.3847/1538-3881/acf7c0 kostenfrei https://doaj.org/article/d35c991048f842f4b9844c174c812a97 kostenfrei https://doi.org/10.3847/1538-3881/acf7c0 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 166 2023 4, p 169
spelling	10.3847/1538-3881/acf7c0 doi (DE-627)DOAJ091857406 (DE-599)DOAJd35c991048f842f4b9844c174c812a97 DE-627 ger DE-627 rakwb eng QB1-991 A. N. Heinze verfasserin aut Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We previously reported a rare class of variable star light curves isolated from a sample of 4.7 million candidate variables from the ATLAS survey. Dubbed “UCBH” light curves, they have broad minima and narrow, symmetrical maxima, with typical periods of 1–10 days and amplitudes of 0.05–0.20 mag. They maintain constant amplitude, shape, and phase coherence over multiple years but do not match any known class of pulsating variables. A localized bright spot near the equator of a rotating star will produce a UCBH-type light curve for most viewing geometries. Most stars that exhibit rotational variability caused primarily by a single bright feature should therefore appear as UCBH stars, although a rotating bright spot is not the only thing that could produce a UCBH-type light curve. We have spectroscopically investigated 14 UCBH stars and found 10 of them to be Ap/Bp stars: A-type or B-type stars with greatly enhanced photospheric abundances of specific heavy elements. Rotationally variable Ap/Bp stars are referred to as α ^2 CVn variables. Most ATLAS UCBH stars are therefore α ^2 CVn stars, although only a minority of α ^2 CVn stars in the literature have UCBH light curves. The fact that α ^2 CVn stars dominate the UCBH class suggests that lone bright spots with sufficient size and contrast develop more readily on Ap/Bp stars than on any other type. The α ^2 CVn UCBH stars may be characterized by a specific magnetic field topology, making them intriguing targets for future Zeeman–Doppler imaging. Peculiar variable stars Chemically peculiar stars Variable stars Magnetic variable stars Ap stars Silicon stars Astronomy Heather Flewelling verfasserin aut Mark E. Huber verfasserin aut In The Astronomical Journal IOP Publishing, 2022 166(2023), 4, p 169 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:166 year:2023 number:4, p 169 https://doi.org/10.3847/1538-3881/acf7c0 kostenfrei https://doaj.org/article/d35c991048f842f4b9844c174c812a97 kostenfrei https://doi.org/10.3847/1538-3881/acf7c0 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 166 2023 4, p 169
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allfieldsGer	10.3847/1538-3881/acf7c0 doi (DE-627)DOAJ091857406 (DE-599)DOAJd35c991048f842f4b9844c174c812a97 DE-627 ger DE-627 rakwb eng QB1-991 A. N. Heinze verfasserin aut Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We previously reported a rare class of variable star light curves isolated from a sample of 4.7 million candidate variables from the ATLAS survey. Dubbed “UCBH” light curves, they have broad minima and narrow, symmetrical maxima, with typical periods of 1–10 days and amplitudes of 0.05–0.20 mag. They maintain constant amplitude, shape, and phase coherence over multiple years but do not match any known class of pulsating variables. A localized bright spot near the equator of a rotating star will produce a UCBH-type light curve for most viewing geometries. Most stars that exhibit rotational variability caused primarily by a single bright feature should therefore appear as UCBH stars, although a rotating bright spot is not the only thing that could produce a UCBH-type light curve. We have spectroscopically investigated 14 UCBH stars and found 10 of them to be Ap/Bp stars: A-type or B-type stars with greatly enhanced photospheric abundances of specific heavy elements. Rotationally variable Ap/Bp stars are referred to as α ^2 CVn variables. Most ATLAS UCBH stars are therefore α ^2 CVn stars, although only a minority of α ^2 CVn stars in the literature have UCBH light curves. The fact that α ^2 CVn stars dominate the UCBH class suggests that lone bright spots with sufficient size and contrast develop more readily on Ap/Bp stars than on any other type. The α ^2 CVn UCBH stars may be characterized by a specific magnetic field topology, making them intriguing targets for future Zeeman–Doppler imaging. Peculiar variable stars Chemically peculiar stars Variable stars Magnetic variable stars Ap stars Silicon stars Astronomy Heather Flewelling verfasserin aut Mark E. Huber verfasserin aut In The Astronomical Journal IOP Publishing, 2022 166(2023), 4, p 169 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:166 year:2023 number:4, p 169 https://doi.org/10.3847/1538-3881/acf7c0 kostenfrei https://doaj.org/article/d35c991048f842f4b9844c174c812a97 kostenfrei https://doi.org/10.3847/1538-3881/acf7c0 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 166 2023 4, p 169
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callnumber-first	Q - Science
author	A. N. Heinze
spellingShingle	A. N. Heinze misc QB1-991 misc Peculiar variable stars misc Chemically peculiar stars misc Variable stars misc Magnetic variable stars misc Ap stars misc Silicon stars misc Astronomy Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars
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topic_title	QB1-991 Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars Peculiar variable stars Chemically peculiar stars Variable stars Magnetic variable stars Ap stars Silicon stars
topic	misc QB1-991 misc Peculiar variable stars misc Chemically peculiar stars misc Variable stars misc Magnetic variable stars misc Ap stars misc Silicon stars misc Astronomy
topic_unstemmed	misc QB1-991 misc Peculiar variable stars misc Chemically peculiar stars misc Variable stars misc Magnetic variable stars misc Ap stars misc Silicon stars misc Astronomy
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title	Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars
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title_full	Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars
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author_browse	A. N. Heinze Heather Flewelling Mark E. Huber
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title_sort	most rotational variables dominated by a single bright feature are α 2 cvn stars
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title_auth	Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars
abstract	We previously reported a rare class of variable star light curves isolated from a sample of 4.7 million candidate variables from the ATLAS survey. Dubbed “UCBH” light curves, they have broad minima and narrow, symmetrical maxima, with typical periods of 1–10 days and amplitudes of 0.05–0.20 mag. They maintain constant amplitude, shape, and phase coherence over multiple years but do not match any known class of pulsating variables. A localized bright spot near the equator of a rotating star will produce a UCBH-type light curve for most viewing geometries. Most stars that exhibit rotational variability caused primarily by a single bright feature should therefore appear as UCBH stars, although a rotating bright spot is not the only thing that could produce a UCBH-type light curve. We have spectroscopically investigated 14 UCBH stars and found 10 of them to be Ap/Bp stars: A-type or B-type stars with greatly enhanced photospheric abundances of specific heavy elements. Rotationally variable Ap/Bp stars are referred to as α ^2 CVn variables. Most ATLAS UCBH stars are therefore α ^2 CVn stars, although only a minority of α ^2 CVn stars in the literature have UCBH light curves. The fact that α ^2 CVn stars dominate the UCBH class suggests that lone bright spots with sufficient size and contrast develop more readily on Ap/Bp stars than on any other type. The α ^2 CVn UCBH stars may be characterized by a specific magnetic field topology, making them intriguing targets for future Zeeman–Doppler imaging.
abstractGer	We previously reported a rare class of variable star light curves isolated from a sample of 4.7 million candidate variables from the ATLAS survey. Dubbed “UCBH” light curves, they have broad minima and narrow, symmetrical maxima, with typical periods of 1–10 days and amplitudes of 0.05–0.20 mag. They maintain constant amplitude, shape, and phase coherence over multiple years but do not match any known class of pulsating variables. A localized bright spot near the equator of a rotating star will produce a UCBH-type light curve for most viewing geometries. Most stars that exhibit rotational variability caused primarily by a single bright feature should therefore appear as UCBH stars, although a rotating bright spot is not the only thing that could produce a UCBH-type light curve. We have spectroscopically investigated 14 UCBH stars and found 10 of them to be Ap/Bp stars: A-type or B-type stars with greatly enhanced photospheric abundances of specific heavy elements. Rotationally variable Ap/Bp stars are referred to as α ^2 CVn variables. Most ATLAS UCBH stars are therefore α ^2 CVn stars, although only a minority of α ^2 CVn stars in the literature have UCBH light curves. The fact that α ^2 CVn stars dominate the UCBH class suggests that lone bright spots with sufficient size and contrast develop more readily on Ap/Bp stars than on any other type. The α ^2 CVn UCBH stars may be characterized by a specific magnetic field topology, making them intriguing targets for future Zeeman–Doppler imaging.
abstract_unstemmed	We previously reported a rare class of variable star light curves isolated from a sample of 4.7 million candidate variables from the ATLAS survey. Dubbed “UCBH” light curves, they have broad minima and narrow, symmetrical maxima, with typical periods of 1–10 days and amplitudes of 0.05–0.20 mag. They maintain constant amplitude, shape, and phase coherence over multiple years but do not match any known class of pulsating variables. A localized bright spot near the equator of a rotating star will produce a UCBH-type light curve for most viewing geometries. Most stars that exhibit rotational variability caused primarily by a single bright feature should therefore appear as UCBH stars, although a rotating bright spot is not the only thing that could produce a UCBH-type light curve. We have spectroscopically investigated 14 UCBH stars and found 10 of them to be Ap/Bp stars: A-type or B-type stars with greatly enhanced photospheric abundances of specific heavy elements. Rotationally variable Ap/Bp stars are referred to as α ^2 CVn variables. Most ATLAS UCBH stars are therefore α ^2 CVn stars, although only a minority of α ^2 CVn stars in the literature have UCBH light curves. The fact that α ^2 CVn stars dominate the UCBH class suggests that lone bright spots with sufficient size and contrast develop more readily on Ap/Bp stars than on any other type. The α ^2 CVn UCBH stars may be characterized by a specific magnetic field topology, making them intriguing targets for future Zeeman–Doppler imaging.
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title_short	Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars
url	https://doi.org/10.3847/1538-3881/acf7c0 https://doaj.org/article/d35c991048f842f4b9844c174c812a97 https://doaj.org/toc/1538-3881
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Most Rotational Variables Dominated by a Single Bright Feature Are α 2 CVn Stars

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