The study of evolutionary changes in intermediate mass magnetic CP stars across the HR diagram Evgeny Semenko Special Astrophysical Observatory of the.

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The study of evolutionary changes in intermediate mass magnetic CP stars across the HR diagram Evgeny Semenko Special Astrophysical Observatory of the Russian Academy of Sciences “Putting A Stars Into Context: Evolution, Environment, and Related Stars” Moscow, SAI MSU

Introduction  Significant magnetic field occurs in a wide range of A and B stars from Ae/Be Herbig objects to the right side of HR diagram.  Young Bp stars generally have stronger magnetic fields with complex structure: HD , HD  There are few Ap stars with strongest magnetic field exceeding 20 kG: HD , HD , BD +00°4535 and some others.  Evolved Ap stars near TAMS are weakly magnetic with practically invisible REEs.

Introduction  Group of evolved stars with accurate measurements of longitudinal magnetic field and other physical parameters consists of at least 6 A stars.  The number of young stars near ZAMS with detailed measurements is quit low. Individual results – individual masses and other parameters.  In order to make detailed study of the evolutional changes of magnetic field and chemical anomalies in Ap/Bp star we need to fill a gap between ZAMS and more evolved objects within one evolutional track.

Introduction All evolved stars are located within the range of solar masses.

Target selection  We carried out an observational program aimed the searches of new magnetic stars and their further detailed study.  Object preselection is based on the next criteria: 1)spectral class from B7 to A0; 2)IR excess along with the absence of any other Ae/Be stars signatures; 3)relatively slow rotation; 4)abundance anomalies.

Instruments  Russian 6-m telescope equipped with: 1.Main stellar spectrograph ( R=0.12 Å/pix, V lim =11.5 m, 500Å sp. range – circular spectropolarimetry. 2.Nasmyth echelle spectrometer ( R=0.026Å/pix, V lim =10 m, Å.  1-m Telescope Zeiss-1000 of the SAO RAS. Low resolution spectroscopy.

An observational sample  About dozen of late B stars were selected as observational candidates.  Polarized spectra obtained for less than half.  Echelle spectra were collected for two objects: HD and HD  Most objects from current sample are winter objects.

The study of magnetic field  Two early Bp stars: HD and HD  Age about 20 million yrs.  SrCrEu-type spectral anomalies.  Rotational velocities are about km/s.

The study of magnetic field Longitudinal magnetic field of HD (left) and HD (right) phased with rotational period. Both periods are smaller than 3 days. Surface field not exceed 3 kG.

Physical parameters of two stars  Effective temperature: K (HD 63347) and K (HD 50341). Derived from photometry and profiles of hydrogen lines.  Surface gravity: 4.2 and 4.1 dex, resp.  Luminocities: 1.64 (HD 63347), 1.60 (HD 50341).  vsin i = 42 km/s (HD 63347), 51 km/s (HD 50341).

Chemical composition of HD Both stars demonstrates strong spectral variability.

Chemical composition of HD 63347

Conclusions  There are stars with weak magnetic fields and prominent chemical peculiarities among young objects.  Overabundance of Fe and Cr in some young stars intrinsically the same as in evolved magnetic stars of equal mass.  While the longitudinal magnetic field of young stars is quite a small, their structure could be more complex than a simple dipole.

Thanks for your attention!