HD 133729: A blue large-amplitude pulsator in orbit around a main-sequence B-type star

Pigulski, A.; Kotysz, K.; Kolaczek-Szymanski, P. A.

doi:10.48550/arxiv.2203.11789

Cited by 3 publications

(8 citation statements)

References 20 publications

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“…However, one object worthy of attention in Table 1 is HD 133729. Pigulski et al (2022) reported a BLAP orbiting the main-sequence B-type star HD 133729 on an orbital period of 23.08433 d. The pulsation period of this BLAP is 32.37 min, with an amplitude 0.21 mag and a rate of period change of −11.5×10 −7 yr −1 , which is consistent with that of known BLAPs. The BLAP nature of the companion to HD 133729 was previously missed due to the dilution of the observed amplitude by the brighter primary.…”

Section: Introductionsupporting

confidence: 77%

“…Except for HD 133729 (Pigulski et al 2022), no evidence for companion stars has been found in BLAPs so far (Pietrukowicz et al 2017;Kupfer et al 2015;Ramsay 2018;McWhirter et al 2020). This however does not necessarily imply that BLAPs are single stars.…”

Section: Formation Channel(s)mentioning

confidence: 95%

“…This however does not necessarily imply that BLAPs are single stars. For example, they could be in long-period binaries which have escaped detection or, otherwise, in short-period binaries, where very bright companions dominate the light budget and dilute the pulsation amplitude (similar to HD 133729, see Pigulski et al 2022). It might also be possible that BLAPs themselves have very faint companions.…”

Section: Formation Channel(s)mentioning

confidence: 99%

See 2 more Smart Citations

Shell helium-burning hot subdwarf B stars as candidates for blue large-amplitude pulsators

Xiong

Casagrande

Chen

et al. 2022

A&A

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Blue large-amplitude pulsators (BLAPs) are a newly discovered type of variable star. Their typical pulsation periods are on the order of a few tens of minutes, with relatively large amplitudes of 0.2-0.4 mag in optical bands, and their rates of period changes are on the order of 10 −7 yr −1 (both positive and negativhe). They are extremely rare objects and attempts to explain their origins and internal structures have attracted a great deal of attention. Previous studies have proposed that BLAPs may be pre-white dwarfs, with masses around 0.3M ⊙ , or core-helium-burning stars in the range of ∼ 0.7−1.1M ⊙ . In this work, we use a number of MESA models to compute and explore whether BLAPs could be explained as shell helium-burning subdwarfs type B (SHeB sdBs). The models that best match existing observational constraints have helium core masses in the range of ∼ 0.45 − 0.5M ⊙ . Our model predicts that the positive rate of period change may evolve to negative. The formation channels for SHeB sdBs involve binary evolution and although the vast majority of BLAPs do not appear to be binaries (with the exception of HD 133729), the observational constraints are still very poor. Motivated by these findings, we explored the Roche lobe overflow channel. Of the 304 binary evolution models we computed, about half of them are able to produce SHeB sdBs in long-period binaries that evade detection from the limited observations that are currently available.

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Section: Introductionsupporting

confidence: 77%

Section: Formation Channel(s)mentioning

confidence: 95%

Section: Formation Channel(s)mentioning

confidence: 99%

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Shell helium-burning hot subdwarf B stars as candidates for blue large-amplitude pulsators

Xiong

Casagrande

Chen

et al. 2022

A&A

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“…The shaded area indicates the approximate range of the gap between classical and high-gravity BLAPs. The new BLAP, HD 133729 [11], was not included here because its pulsation amplitude was not obtained directly from light curves.…”

mentioning

confidence: 99%

“…Rate of period change. BLAPs are believed to stem from either heliumcore pre-white-dwarfs (pre-WDs) or core helium-burning (CHeB) subdwarfs [1,2,[4][5][6]11], since stars formed from these two channels cover the BLAP region in the Hertzsprung-Russell (HR) diagram. The pre-WDs usually contract with the cooling process while the CHeB stars will burn helium steadily on nuclear timescales.…”

mentioning

confidence: 99%

An 18.9 min blue large-amplitude pulsator crossing the ‘Hertzsprung gap’ of hot subdwarfs

Lin

Wang

et al. 2022

Nat Astron

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Blue large-amplitude pulsators (BLAPs) represent a new and rare class of hot pulsating stars with unusually large amplitudes and short periods. Up to now, only 21 confirmed BLAPs have been identified from more than one billion monitored stars, including a group with pulsation period longer than 20 min (classical BLAPs; [1]) and the other group with pulsation period below 10 min (high-gravity BLAPs; [2]). The evolutionary path that could give rise to such kinds of stellar configurations is unclear. Here we report on a comprehensive study of the peculiar BLAP discovered by the Tsinghua University -Ma Huateng Telescopes for Survey (TMTS) [3], TMTS J035143.63+584504.2 (TMTS-BLAP-1); it is the first confirmed BLAP located within the "period gap" between high-gravity and classical BLAPs. This new BLAP has an 18.9 min pulsation period, and is similar to the classical BLAPs with an extended helium-enriched envelope. In particular, the long-term monitoring data of TMTS-BLAP-1 reveal that this pulsating star has an unusually large rate of period change, Ṗ /P = 2.3 × 10 −6 yr −1 . Such a significant and positive value challenges the scenarios of both the helium-core pre-white-dwarf and the core-helium burning [1, 2, 4-6]), but is consistent with that derived from shell-helium burning. The particular pulsation period and unusual rate of period change indicate that TMTS-BLAP-1 is at a short-lived (∼ 10 6 yr) phase of shell-helium ignition before the stable shell-helium burning; in other words, TMTS-BLAP-1 is going through a "Hertzsprung gap" of hot subdwarfs. This demonstrates that hot subdwarf stars have a similar evolutionary fate as main-sequence stars; some subdwarfs can leave their "main-sequence" stage and appear as diverse pulsating variables in distinct regions of the Hertzsprung-Russell diagram, thereby opening a new window for explorations of rare pulsating stars that evolved from stripped-envelope stars.The minute-cadence observations by Tsinghua University -Ma Huateng Telescopes for Survey (TMTS) enable the search of variable stars with periods shorter than 1 hr. TMTS J035143.63+584504.2 is such a newly discovered short-period variable, having an 18.9 min period and a peak-to-peak amplitude up to ∼ 0.3 mag in white light [3]. Follow-up observations with SNOVA,

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An 18.9-minute Blue Large-Amplitude Pulsator Crossing the "Hertzsprung Gap'' of Hot Subdwarfs

Lin

Németh

et al. 2022

Preprint

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Blue large-amplitude pulsators (BLAPs) represent a new and rare class of hot pulsating stars with unusually large amplitudes and short periods. Up to now, only 21 confirmed BLAPs have been identified from more than one billion monitored stars, including a group with pulsation period longer than 20 min (classical BLAPs; [1]) and the other group with pulsation period below 10 min (high-gravity BLAPs; [2]). The evolutionary path that could give rise to such kinds of stellar configurations is unclear. Here we report on a comprehensive study of the peculiar BLAP discovered by the Tsinghua University – Ma Huateng Telescopes for Survey (TMTS) [3], TMTS J035143.63+584504.2 (TMTSBLAP-1); it is the first confirmed BLAP located within the “period gap” between high-gravity and classical BLAPs. This new BLAP has an 18.9 min pulsation period, and is similar to the classical BLAPs with an extended helium-enriched envelope. In particular, the long-term monitoring data of TMTS-BLAP-1 reveal that this pulsating star has an unusually large rate of period change, ˙P /P = 2.3 × 10−6 yr−1. Such a significant and positive value challenges the scenarios of both the helium-core pre-white-dwarf and the core-helium burning [1, 2, 4–6]), but is consistent with that derived from shell-helium burning. The particular pulsation period and unusual rate of period change indicate that TMTS-BLAP-1 is at a short-lived (∼ 106 yr) phase of shell-helium ignition before the stable shell-helium burning; in other words, TMTSBLAP-1 is going through a “Hertzsprung gap” of hot subdwarfs. This demonstrates that hot subdwarf stars have a similar evolutionary fate as main-sequence stars; some subdwarfs can leave their “main-sequence” stage and appear as diverse pulsating variables in distinct regions of the Hertzsprung-Russell diagram, thereby opening a new window for explorations of rare pulsating stars that evolved from stripped-envelope stars.

show abstract

HD 133729: A blue large-amplitude pulsator in orbit around a main-sequence B-type star

Cited by 3 publications

References 20 publications

Shell helium-burning hot subdwarf B stars as candidates for blue large-amplitude pulsators

Shell helium-burning hot subdwarf B stars as candidates for blue large-amplitude pulsators

An 18.9 min blue large-amplitude pulsator crossing the ‘Hertzsprung gap’ of hot subdwarfs

An 18.9-minute Blue Large-Amplitude Pulsator Crossing the "Hertzsprung Gap'' of Hot Subdwarfs

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