Rotational velocities of A-type stars ?;?? I. Measurement of v sini in the southern hemisphere

@article{Royer2001RotationalVO,
  title={Rotational velocities of A-type stars ?;?? I. Measurement of v sini in the southern hemisphere},
  author={Fr{\'e}d{\'e}ric Royer and Michele Marie Gerbaldi and Rosanna Faraggiana and Ana E. G{\'o}mez},
  journal={Astronomy and Astrophysics},
  year={2001},
  volume={381},
  pages={105-121}
}
Within the scope of a Key Programme determining fundamental parameters of stars observed by HIPPARCOS, spectra of 525 B8 to F2-type stars brighter than V = 8 have been collected at ESO. Fourier transforms of several line proles in the range 4200{4500 A are used to derive v sini from the frequency of the rst zero. Statistical analysis of the sample indicates that measurement error is a function of v sini and this relative error of the rotational velocity is found to be about 6% on average. The… 

Rotational Velocity Distributions of A-Type Main-Sequence Stars

The different velocity distributions (v sin i, and v) are determined for single, non peculiar, A-type main-sequence stars, using homogeneous data. These distributions, together with synthetic

Rotational Velocities of Southern B Stars and a Statistical Discussion of the Rotational Properties

We have measured the projected rotational velocities of 1023 southern B stars listed in the Bright Star Catalog (BSC) and calibrated them against the 1975 Slettebak et al. system. We joined the

The interferometric diameter and internal structure of Sirius A

The interferometric observations of dwarf stars in the solar neighbourhood, combined with Hipparcos parallaxes provide very precise values of their linear diameters. In this paper, we report the

Rotational Velocities of B Stars

We measured the projected rotational velocities of 1092 northern B stars listed in the Bright Star Catalogue (BSC) and calibrated them against the 1975 Slettebak et al. system. We found that the

Fourier method of determining the rotational velocities in OB stars

Aims. We present a comprehensive study that applies the Fourier transform to a sample of O and early B-type stars (either dwarfs, giants, or supergiants) to determine their projected rotational

Spectroscopic and photometric analysis of NSV 24512: an early-type eclipsing binary embedded in a dust cloud

We present differential V-band photometric observations and the first radial velocities of NSV 24512, which is embedded in the Serpens star-forming region. This double-lined system has an eccentric

VLTI near-IR interferometric observations of Vega-like stars: Radius and age of a PsA, b Leo, b Pic, e Eri and t Cet

We report in this paper the direct interferometric measurement of the angular diameter of five nearby Vega-like stars: α PsA, β Leo, β Pic, � Eri and τ Cet. The near-infrared (K and H bands)

ROTATION AND SURFACE ABUNDANCE PECULIARITIES IN A-TYPE STARS

In an attempt of clarifying the connection between the photospheric abundance anomalies and the stellar rotation as well as of exploring the nature of “normal A” stars, the abundances of seven

Rotational velocities of A-type stars. III. Velocity distributions

Aims. A sample of $v\sin i$ of B9 to F2-type main sequence single stars has been built from highly homogeneous ${v\sin i}$ parameters determined for a large sample cleansed of objects presenting the

Rotational velocities of A-type stars - IV. Evolution of rotational velocities

Context. In previous works of this series, we have shown that late B- and early A-type stars have genuine bimodal distributions of rotational velocities and that late A-type stars lack slow rotators.
...

References

SHOWING 1-10 OF 57 REFERENCES

Radial velocities of HIPPARCOS southern B8-F2 type stars

Radial velocities have been determined for a sample of B8-F2 type stars observed by the Hipparcos satellite. Observations were obtained within the frame- work of an ESO key-program. Radial velocities

ROTATIONAL VELOCITIES OF LATE-TYPE STARS

A calibration based on the results of Gray has been used to determine projected rotational velocities for 133 bright stars with spectral types of F, G, or K, most of which appear in {The Bright Star

Applications of Fourier analysis to broadening of stellar line profiles. II. A saturated line in 32 Aquarii and in Sirius.

An application of Gray's Ftheier analysis technique demonstrates that the shape of the Fe i lambda4476 profile in 32 Agr is consistent with a Gaussian microturbulent velocity field in the atmosphere

Newly identified main-sequence A stars with circumstellar dust

The IRAS Faint Source Survey data base and the ADDSCAN/SCANPI software are used to search for systems with circumstellar dust in two samples: all of the 62 A stars in Woolley's catalog, which lie

Search for reference A0 dwarf stars: Masses and luminosities revisited with HIPPARCOS parallaxes

Hipparcos data for 71 nearby dwarf A0 stars were combined with other data, in particular with high resolution spectra to establish the HR diagram in this temperature range. Almost 30% of unknown

THE ANGULAR MOMENTUM OF MAIN SEQUENCE STARS AND ITS RELATION TO STELLAR ACTIVITY

Rotational velocities are reported for intermediate-mass main sequence stars it the field. The measurements are based on new, high S/N CCD spectra from the Coudé Feed Telescope of the Kitt Peak

Rotational velocities of low-mass stars in the Hyades

High-resolution echelle spectra have been used to estimate rotational velocities for K and M dwarfs in the Hyades. All of the K dwarfs have rotational velocities less than the instrumental limit of

The application of a Bessel transform to the determination of stellar rotational velocities

A method for analysing line profiles by means of a transform using Bessel functions is described. This yields the stellar rotational velocityv sini, to an accuracy of about ±1 km s−1 for rotational

γ Doradus Stars: Defining a New Class of Pulsating Variables

In this paper we describe a new class of pulsating stars, the prototype of which is the bright, early, F‐type dwarf γ Doradus. These stars typically have between 1 and 5 periods ranging from 0.4 to 3
...