The interferometric diameter and internal structure of Sirius A

@article{Kervella2003TheID,
  title={The interferometric diameter and internal structure of Sirius A},
  author={Pierre Kervella and F. Th{\'e}venin and P. Morel and Pascal J. Bord{\'e} and Emmanuel di Folco},
  journal={arXiv: Astrophysics},
  year={2003}
}
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 direct measurement of the angular diameter of the bright star Sirius A with the VINCI/VLTI instrument. We obtain a uniform disk angular diameter of UD = 5.936 +/- 0.016 mas in the K band and a limb darkened value of LD = 6.039 +/- 0.019 mas. In combination with the Hipparcos parallax of 379.22 +/- 1.58… 

Figures and Tables from this paper

The Angular Diameter and Fundamental Parameters of Sirius A

The Sydney University Stellar Interferometer (SUSI) has been used to make a new determination of the angular diameter of Sirius A. The observations were made at an effective wavelength of 694.1 nm

Pseudomagnitudes and Differential Surface Brightness: Application to the apparent diameter of stars

The diameter of a star is a major observable that serves to test the validity of stellar structure theories. It is also a difficult observable that is mostly obtained with indirect methods since the

VINCI / VLTI observations of Main Sequence stars

Main Sequence (MS) stars are by far the most numerous class in the Universe. They are often somewhat neglected as they are relatively quiet objects (but exceptions exist), though they bear testimony

The Angular Diameter of λ Boötis

Using the CHARA Array and the Palomar Testbed Interferometer, the chemically peculiar star λ Boötis has been spatially resolved. We have measured the limb darkened angular diameter to be θLD = 0.533

The Sirius System and Its Astrophysical Puzzles: Hubble Space Telescope and Ground-based Astrometry

Sirius, the seventh-nearest stellar system, is a visual binary containing the metallic-line A1 V star Sirius A, the brightest star in the sky, orbited in a 50.13 year period by Sirius B, the

The angular sizes of dwarf stars and subgiants (Research Note) Non-linear surface brightness relations in BVRcIc from interferometry

Context. The prediction of stellar angular diameters from broadband photometry plays an important role in different applications. In particular, long-baseline interferometry, gravitational

Predicting stellar angular diameters from V, I C , H and K photometry

Determining the physical properties of microlensing events depends on having accurate angular sizes of the source star. Using long-baseline optical interferometry we are able to measure the angular

MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary

We report on the observations, analysis and interpretation of the microlensing event MOA-2019-BLG-008. The observed anomaly in the photometric light curve is best described through a binary lens

The diameter and evolutionary state of Procyon A. Multi-technique modeling using asteroseismic and i

We report the angular diameter measurement obtained with the VINCI/VLTI instrument on the nearby star Procyon A ( α  CMi A, F5IV–V), at a relative precision of ± 0.9%. We obtain a uniform disk

The radii of the nearby K5V and K7V stars 61 Cygni A & B. CHARA/FLUOR interferometry and CESAM2k modeling

Context: The main sequence binary star 61 Cyg (K5V+K7V) is our nearest stellar neighbour in the northern hemisphere. This proximity makes it a particularly well suited system for very high accuracy
...

References

SHOWING 1-10 OF 42 REFERENCES

The diameters of $\alpha$ Centauri A and B - A comparison of the asteroseismic and VINCI/VLTI views

We compare the first direct angular diameter measurements obtained on our closest stellar neighbour, Centauri, to recent model diameters constrained by asteroseismic observations. Using the VINCI

Sirius B: A New, More Accurate View

The mass and radius for Sirius B are found to be consistent with the theoretical mass-radius relation for a carbon-core white dwarf.

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

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

New determination of the angular diameter of Sirius

We report a new determination of the angular size of α CMa (Sirius), which has yielded an equivalent uniform disk diameter of 5.63 ±0.08 arc ms. This result represents the first measurement of a

Direct multi-wavelength limb-darkening measurements of three late-type giants with the Navy Prototype Optical Interferometer

We present direct measurements of the limb-darkened intensity proles of the late-type giant stars HR 5299, HR 7635, and HR 8621 obtained with the Navy Prototype Optical Interferometer (NPOI) at the

The accurate determination of stellar angular diameters using broad-band stellar interferometry

The angular diameter of a star can be estimated from interferometric observations by fitting the data with the visibility function for a uniformly illuminated disc and then using published correction

Analysis of solar radius determination obtained by the modern CCD astrolabe of the Calern Observatory - A new approach of the solar limb definition

A semi-empirical model of solar images is presented here and used to derive the solar radius from astrolabe observations made at the Cote d'Azur Observatory (OCA), at the Calern station. This model

The Abundance Patterns of Sirius and Vega

On the basis of high-resolution echelle spectra obtained with the Coudé Echelle Spectrograph attached to the 2.16 m telescope at the Beijing Astronomical Observatory (Xinglong, China) for Sirius and

Testing the White Dwarf Mass-Radius Relation with Hipparcos

We present the Hipparcos parallaxes and resulting radii for 10 white dwarfs in visual binaries or common proper-motion systems and 11 field white dwarfs. For bright stars, Hipparcos parallaxes have

Limb-darkening corrections for interferometric uniform disc stellar angular diameters

Stellar angular diameters determined interferometrically are generally established by fitting the observed visibility data with a curve appropriate for a uniformly illuminated disc. The resulting