Magnetic field of CP stars in the Ori OB1 association. II. HD36540, HD36668, HD36916, HD37058

Romanyuk, I. I.; Semenko, E. A.; Yakunin, I. A.; Kudryavtsev, D. O.; Moiseeva, A. V.

doi:10.1134/s1990341317020079

Cited by 18 publications

(11 citation statements)

References 24 publications

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“…The obtained B e values ranged from −2100 to +2000 G. We carried out eight observations of the star. Measurements of the Zeeman effect in the metal and hydrogen lines confirm the presence of a strong field, but its variation limits are much larger than those published by Romanyuk et al (2017).…”

Section: Hd 36313 = V1093 Orionmentioning

confidence: 58%

“…In our research program, we decided to measure magnetic fields of all chemically peculiar * roman@sao.ru stars in the Orion OB1 association with reliably determined ages of its individual subgroups. This article continues the series of our papers (Romanyuk et al 2014(Romanyuk et al , 2015(Romanyuk et al , 2013(Romanyuk et al , 2017 for complex investigation of magnetic chemically peculiar stars in Orion. The objectives of the program were presented in Romanyuk et al (2013), the observation and data analysis method was described in Romanyuk et al (2014Romanyuk et al ( , 2015Romanyuk et al ( , 2017.…”

Section: Introductionmentioning

confidence: 72%

“…This article continues the series of our papers (Romanyuk et al 2014(Romanyuk et al , 2015(Romanyuk et al , 2013(Romanyuk et al , 2017 for complex investigation of magnetic chemically peculiar stars in Orion. The objectives of the program were presented in Romanyuk et al (2013), the observation and data analysis method was described in Romanyuk et al (2014Romanyuk et al ( , 2015Romanyuk et al ( , 2017.…”

Section: Introductionmentioning

confidence: 72%

“…The columns of the table present: the number of the star in the HD catalog; the Julian date of an observation; the signal-to-noise ratio S/N ; the longitudinal magnetic field in gauss, obtained using the modified Babcock method (B e (z),) the regression method (B e (r)), and by the Hβ hydrogen line (B e (h)); the corresponding root-mean-square errors σ. The magnetic-field measurement method is described in detail in the previous papers (Romanyuk et al 2014(Romanyuk et al , 2015(Romanyuk et al , 2017. For sixteen stars, we obtained a total of 110 magnetic field measurements, at least five for each object.…”

Section: Measurementsmentioning

confidence: 99%

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Magnetic Fields of CP Stars in the Orion OB1 Association. IV. Stars of Subgroup 1b

et al. 2021

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The paper presents magnetic field measurements for 15 chemically peculiar (CP) stars of subgroup 1b in the Orion OB1 association. We have found that the proportion of stars with strong magnetic fields among these 15 CP stars is almost twice as large as in subgroup 1a. Along with this, the age of subgroup 1b is estimated as 2 Myr, and the age of subgroup 1a is in the order of 10 Myr. The average root-mean-square magnetic field B e (all) for stars in subgroup 1b is 2.3 times higher than that for stars in subgroup 1a. The conclusions obtained fall within the concept of the fossil origin of large-scale magnetic fields in B and A stars, but the rate of field weakening with age appears anomalously high. We present our results as an important observational test for calibrating the theory of stellar magnetic field formation and evolution.

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Section: Hd 36313 = V1093 Orionmentioning

confidence: 58%

Section: Introductionmentioning

confidence: 72%

Section: Introductionmentioning

confidence: 72%

Section: Measurementsmentioning

confidence: 99%

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Magnetic Fields of CP Stars in the Orion OB1 Association. IV. Stars of Subgroup 1b

et al. 2021

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“…Our measurements were made using the 6‐m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (see, e.g., Romanyuk et al ). We obtained more than 500 Zeeman spectra for 55 stars, the measurements having been partially published earlier: see Yakunin (); Semenko et al (); Romanyuk et al (); Romanyuk et al (). Usually we used two methods of magnetic field measurements: (1) classical Zeeman spectroscopy (Babcock ) modified for the reduction of charge‐coupled device (CCD) images (Kudryavtsev et al ), and (2) the regression method developed by Bagnulo et al ().…”

Section: Magnetic Field Of Ap/bp Stars In Orion Ob1mentioning

confidence: 99%

Magnetic chemically peculiar stars in the Orion OB1 association

et al. 2017

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We discuss an ongoing project on the investigation of magnetic fields of chemically peculiar (CP) stars in the Orion OB1 association. More than 500 polarized spectra for 55 stars have been obtained with the Russian 6‐m telescope. We found eight new magnetic stars in addition to the 20 previously known. The frequency of Ap/Bp stars among normal A and B stars and the frequency of magnetic stars among all Ap/Bp stars decrease with age in the Orion OB1 association.

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MOBSTER – VI. The crucial influence of rotation on the radio magnetospheres of hot stars

Shultz

Owocki

ud‐Doula

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Numerous magnetic hot stars exhibit gyrosynchrotron radio emission. The source electrons were previously thought to be accelerated to relativistic velocities in the current sheet formed in the middle magnetosphere by the wind opening magnetic field lines. However, a lack of dependence of radio luminosity on the wind power, and a strong dependence on rotation, has recently challenged this paradigm. We have collected all radio measurements of magnetic early-type stars available in the literature. When constraints on the magnetic field and/or the rotational period are not available, we have determined these using previously unpublished spectropolarimetric and photometric data. The result is the largest sample of magnetic stars with radio observations that has yet been analyzed: 131 stars with rotational and magnetic constraints, of which 50 are radio-bright. We confirm an obvious dependence of gyrosynchrotron radiation on rotation, and furthermore find that accounting for rotation neatly separates stars with and without detected radio emission. There is a close correlation between Hα emission strength and radio luminosity. These factors suggest that radio emission may be explained by the same mechanism responsible for Hα emission from centrifugal magnetospheres, i.e. centrifugal breakout (CBO), however, whereas the Hα-emitting magnetosphere probes the cool plasma before breakout, radio emission is a consequence of electrons accelerated in centrifugally-driven magnetic reconnection.

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Magnetic field of CP stars in the Ori OB1 association. II. HD36540, HD36668, HD36916, HD37058

Cited by 18 publications

References 24 publications

Magnetic Fields of CP Stars in the Orion OB1 Association. IV. Stars of Subgroup 1b

Magnetic Fields of CP Stars in the Orion OB1 Association. IV. Stars of Subgroup 1b

Magnetic chemically peculiar stars in the Orion OB1 association

MOBSTER – VI. The crucial influence of rotation on the radio magnetospheres of hot stars

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