750 research outputs found
Evolution of magnetic fields in stars across the upper main sequence: I. Catalogue of magnetic field measurements with FORS1 at the VLT
To properly understand the physics of Ap and Bp stars it is particularly
important to identify the origin of their magnetic fields. For that, an
accurate knowledge of the evolutionary state of stars that have a measured
magnetic field is an important diagnostic. Previous results based on a small
and possibly biased sample suggest that the distribution of magnetic stars with
mass below 3 M_sun in the H-R diagram differs from that of normal stars in the
same mass range (Hubrig et al. 2000). In contrast, higher mass magnetic Bp
stars may well occupy the whole main-sequence width (Hubrig, Schoeller & North
2005). In order to rediscuss the evolutionary state of upper main sequence
magnetic stars, we define a larger and bias-free sample of Ap and Bp stars with
accurate Hipparcos parallaxes and reliably determined longitudinal magnetic
fields. We used FORS1 at the VLT in its spectropolarimetric mode to measure the
magnetic field in chemically peculiar stars where it was unknown or poorly
known as yet. In this first paper we present our results of the mean
longitudinal magnetic field measurements in 136 stars. Our sample consists of
105 Ap and Bp stars, two PGa stars, 17 HgMn stars, three normal stars, and nine
SPB stars. A magnetic field was for the first time detected in 57 Ap and Bp
stars, in four HgMn stars, one PGa star, one normal B-type star and four SPB
stars.Comment: 9 pages, 2 figures, 2 tables, to appear in AN 327, 28
Searching for a link between the presence of chemical spots on the surface of HgMn stars and their weak magnetic fields
We present the results of mapping the HgMn star AR Aur using the Doppler
Imaging technique for several elements and discuss the obtained distributions
in the framework of a magnetic field topology.Comment: 2 pages, 1 figure, to appear in Proceedings of IAU Symposium 259
"Cosmic Magnetic Fields: from Planets, to Stars and Galaxies", Tenerife,
Spain, November 3-7, 200
Characterising the magnetic fields of the Herbig Ae/Be stars HD97048, HD150193, HD176386, and MWC480
Our knowledge of the presence and the role of magnetic fields in
intermediate-mass pre-main-sequence stars remains very poor.
We present the magnetic properties of four Herbig Ae/Be stars that have not
been previously studied in detail.
Our results for the three Herbig Ae/Be stars HD97048, HD150193, and HD176386
are based on multi-epoch low-resolution spectra obtained in spectropolarimetric
mode with FORS2 mounted on the VLT. New high-resolution polarimetric spectra
were obtained for MWC480 with the SOFIN spectrograph installed at the Nordic
Optical Telescope. We discuss 41 FORS2 low-resolution observations of the
Herbig Ae/Be stars HD97048, HD150193, and HD176386 and determine their
rotational periods. Using stellar fundamental parameters and the longitudinal
magnetic field phase curves, we place constraints on the magnetic field
geometry. Three high-resolution circularly polarised SOFIN spectra obtained for
MWC480 were measured using the moment technique where wavelength shifts between
right- and left-hand side circularly polarised spectra are interpreted in terms
of a longitudinal magnetic field .
Our search for periodicities resulted in P=0.693d for HD97048, P=1.317d for
HD150193, and P=0.899d for HD176386. The magnetic field geometry can likely be
described by a centred dipole with a polar magnetic field strength B_d of
several hundred Gauss. The longitudinal magnetic-field measurements of MWC480
reveal the presence of a strong kG field, which was undetected in our previous
low-resolution polarimetric observations with FORS1. A weak magnetic field was
detected in the circumstellar components of the Ca II H&K lines and the Na I D
lines, indicating a complex interaction between the stellar magnetic field and
the circumstellar environment.Comment: 8 pages, 9 figures, 5 tables, accepted for publication in A&
Dynamical evolution of titanium, strontium, and yttrium spots on the surface of the HgMn star HD 11753
Aims. We gathered about 100 high-resolution spectra of three typical HgMn
(mercury-manganese) stars, HD 11753, HD 53244, and HD 221507, to search for
slowly pulsating B-like pulsations and surface inhomogeneous distribution of
various chemical elements. Methods. Classical frequency analysis methods were
used to detect line profile variability and to determine the variation period.
Doppler imaging reconstruction was performed to obtain abundance maps of
chemical elements on the stellar surface. Results. For HD 11753, which is the
star with the most pronounced variability, distinct spectral line profile
changes were detected for Ti, Sr, Y, Zr, and Hg, whereas for HD 53244 and HD
221507 the most variable line profiles belong to the elements Hg and Y,
respectively. We derived rotation periods for all three stars from the
variations of radial velocities and equivalent widths of spectral lines
belonging to inhomogeneously distributed elements: P_rot (HD 11753)=9.54 d,
P_rot (HD 53244)=6.16 d, and P_rot (HD 221507)=1.93 d. For HD 11753 the Doppler
imaging technique was applied to derive the distribution of the most variable
elements Ti, Sr, and Y using two datasets separated by ~65 days. Results of
Doppler imaging reconstruction revealed noticeable changes in the surface
distributions of TiII, SrII, and YII between the datasets, indicating the
hitherto not well understood physical processes in stars with radiative
envelopes that cause a rather fast dynamical chemical spot evolution.Comment: Accepted for publication in Astronomy and Astrophysics, 6 pages, 9
figures, 2 tables
Recent studies of magnetic fields in Herbig Ae/Be stars
New determinations of the mean longitudinal magnetic field for several Herbig Ae/Be stars are presented. The longitudinal magnetic field measurements of MWC 480 reveal the presence of a strong kG field, which was undetected in our previous low‐resolution polarimetric observations with FORS 1. The magnetic field geometries of Herbig Ae/Be stars studied with spectropolarimetric time series can likely be described by centred dipoles with polar magnetic field strengths of several hundred Gauss. A number of Herbig Ae/Be stars with detected magnetic fields were recently observed with X‐shooter in the visible and near‐IR as well as with the high‐resolution near‐IR spectrograph CRIRES. These observations are of great importance to understand the relation between the magnetic field topology and the physics of accretion flow and accretion disk gas emission (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/89448/1/1022_ftp.pd
The narrow, inner CO ring around the magnetic Herbig Ae star, HD 101412
We describe and model emission lines in the first overtone band of CO in the
magnetic Herbig Ae star HD 101412. High-resolution CRIRES spectra reveal
unusually sharp features which suggest the emission is formed in a thin disk
centered at 1 AU with a width 0.32 AU or less. A wider disk will not fit the
observations. Previous observations have reached similar conclusions, but the
crispness of the new material brings the emitting region into sharp focus.Comment: Accepted as Astronomy and Astrophysics Letter; 4 pages, 5 figure
Magnetic fields in O-type stars measured with FORS1 at the VLT
The presence of magnetic fields in O-type stars has been suspected for a long
time. The discovery of such fields would explain a wide range of well
documented enigmatic phenomena in massive stars, in particular cyclical wind
variability, Halpha emission variations, chemical peculiarity, narrow X-ray
emission lines and non-thermal radio/X-ray emission. Here we present the
results of our studies of magnetic fields in O-type stars, carried out over the
last years.Comment: 2 pages, 1 figure, to appear in Proceedings of IAU Symposium 259
"Cosmic Magnetic Fields: from Planets, to Stars and Galaxies", Tenerife,
Spain, November 3-7, 200
Discovery of magnetic fields in three He variable Bp stars with He and Si spots
It is essential for the understanding of stellar structure models of high
mass stars to explain why constant stars, non-pulsating chemically peculiar hot
Bp stars and pulsating stars co-exist in the slowly pulsating B stars and beta
Cephei instability strips. We have conducted a search for magnetic fields in
the four Bp stars HD55522, HD105382, HD131120, and HD138769 which previously
have been wrongly identified as slowly pulsating B stars. A recent study of
these stars using the Doppler Imaging technique revealed that the elements He
and Si are inhomogeneously distributed on the stellar surface, causing the
periodic variability. Using FORS1 in spectropolarimetric mode at the VLT, we
have acquired circular polarisation spectra to test the presence of a magnetic
field in these stars. A variable magnetic field is clearly detected in HD55522
and HD105382, but no evidence for the existence of a magnetic field was found
in HD131120. The presence of a magnetic field in HD138769 is suggested by one
measurement at 3 sigma level. We discuss the occurence of magnetic B stars
among the confirmed pulsating B stars and find strong magnetic fields of order
kG and oscillations to be mutually exclusive.Comment: 5 pages, 3 figures, 2 tables, accepted for publication in A
Is the Wind of the Galactic Oe Star HD 155806 Magnetically Confined?
Spectropolarimetric observations of HD 155806 - the hottest Galactic Oe star
- were obtained with CFHT/ESPaDOnS to test the hypothesis that disk signatures
in its spectrum are due to magnetic channeling and confinement of its stellar
wind. We did not detect a dipole field of sufficient strength to confine the
wind, and could not confirm previous reports of a magnetic detection. It
appears that stellar magnetism is not responsible for producing the disk of HD
155806.Comment: 2 pages, 1 figure; to appear in the proceedings of IAU Symposium 27
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