Limb-darkening corrections for interferometric uniform disc stellar angular diameters

Davis, John; Tango, W. J.; Booth, A. J.

doi:10.1046/j.1365-8711.2000.03701.x

Cited by 77 publications

(107 citation statements)

References 13 publications

Supporting

Mentioning

107

Contrasting

Order By: Relevance

“…This is especially true when the measured visibilities do not probe the second lobe. Davis et al (2000) measured stellar angular diameters from interferometric observations by assuming that the stellar intensity profile is uniform, i.e. the intensity at any point on a stellar disk is equal to the central intensity.…”

Section: Angular Diameter Correctionsmentioning

confidence: 99%

“…In that case, the uniform-disk angular diameter can be directly fit to the observed visibilities and then converted to a limb-darkened angular diameter using model stellar atmospheres. Davis et al (2000) computed corrections using plane-parallel ATLAS models (Kurucz 1993) and found k ≡ θ UD /θ LD = 0.91 to 0.98 in the wavelength range λ = 400-800 nm. These limb-darkening corrections have been applied to observations of Cepheids (Gallenne et al 2012) and Sirius (Davis et al 2011) for example.…”

Section: Angular Diameter Correctionsmentioning

confidence: 99%

See 1 more Smart Citation

Spherically-symmetric model stellar atmospheres and limb darkening

Neilson

Lester

2013

A&A

View full text Add to dashboard Cite

Model stellar atmospheres are fundamental tools for understanding stellar observations from interferometry, microlensing, eclipsing binaries and planetary transits. However, the calculations also include assumptions, such as the geometry of the model. We use intensity profiles computed for both plane-parallel and spherically symmetric model atmospheres to determine fitting coefficients in the BVRIHK, CoRot and Kepler wavebands for limb darkening using several different fitting laws, for gravity-darkening and for interferometric angular diameter corrections. Comparing predicted variables for each geometry, we find that the spherically symmetric model geometry leads to different predictions for surface gravities log g < 3. In particular, the most commonly used limb-darkening laws produce poor fits to the intensity profiles of spherically symmetric model atmospheres, which indicates the need for more sophisticated laws. Angular diameter corrections for spherically symmetric models range from 0.67 to 1, compared to the much smaller range from 0.95 to 1 for plane-parallel models.

show abstract

Section: Angular Diameter Correctionsmentioning

confidence: 99%

Section: Angular Diameter Correctionsmentioning

confidence: 99%

Spherically-symmetric model stellar atmospheres and limb darkening

Neilson

Lester

2013

A&A

View full text Add to dashboard Cite

show abstract

“…When comparing observations with in a broad-band filter, particular attention must be paid to the smearing effect (also known as bandwidth smearing) affecting the measurements (Davis et al 2000;Kervella et al 2003;Verhoelst 2005). This is the chromatic aberration caused by observations never being monochromatic but integrated over a certain wavelength range defined by the broad-band filter curve.…”

Section: Synthetic Profiles For Broad-band Filtersmentioning

confidence: 99%

Interferometric properties of pulsating C-rich AGB stars

Paladini¹,

Aringer²,

Hron³

et al. 2009

A&A

View full text Add to dashboard Cite

Aims. On the basis of a set of dynamic model atmospheres of C-rich AGB stars, we present the first theoretical study of centre-to-limb variation (CLV) properties and relative radius interpretation on narrow and broad-band filters. We computed visibility profiles and the equivalent uniform disc (UD) radii to investigate the dependence of these quantities on the wavelength and pulsation phase. Methods. After an accurate morphological analysis of the visibility and intensity profiles determined in narrow and broad-band filters, we fitted our visibility profiles with a UD function simulating the observational approach. The UD-radii were computed using three different fitting-methods to investigate the influence of the visibility sampling profile: single point, two points and a least squares method. Results. The intensity and visibility profiles of models characterises by mass loss show a behaviour very different from a UD. We found that UD-radii are wavelength dependent and that this dependence is stronger if mass loss is present. Strong opacity contributions from C 2 H 2 affect all radius measurements at 3 μm and in the N-band, resulting in higher values for the UD-radii. In the case of models with mass loss the predicted behaviour of UD-radii versus phase is complicated, while the radial changes are almost sinusoidal for models without mass loss. Compared to the M-type stars, for the C-stars no windows are available for measuring the pure continuum.

show abstract

“…Claret (2000), considering the physical parameters of Car detailed in Paper I (T eff , log g, ...). The visibility model is computed taking into account the bandwidth smearing effect (Davis et al 2000;Kervella et al 2004a) that is due to the broadband operation of VINCI. This is one of the simplest models to account for the contribution of a diffuse CSE, together with the photospheric emission from the star itself.…”

Section: K Band Modelmentioning

confidence: 99%

Extended envelopes around Galactic Cepheids

Kervella¹,

Mérand²,

Perrin³

et al. 2006

A&A

106

View full text Add to dashboard Cite

We present the results of long-baseline interferometric observations of the bright southern Cepheid Carinae in the infrared N (8−13 µm) and K (2.0−2.4 µm) bands, using the MIDI and VINCI instruments of the VLT Interferometer. We resolve in the N band a large circumstellar envelope (CSE) that we model with a Gaussian of 3 R (≈500 R ≈ 2−3 AU) half width at half maximum. The signature of this envelope is also detected in our K band data as a deviation from a single limb darkened disk visibility function. The superimposition of a Gaussian CSE on the limb darkened disk model of the Cepheid star results in a significantly better fit of our VINCI data. The extracted CSE parameters in the K band are a half width at half maximum of 2 R , comparable to the N band model, and a total brightness of 4% of the stellar photosphere. A possibility is that this CSE is linked to the relatively large mass loss rate of Car. Though its physical nature cannot be determined from our data, we discuss an analogy with the molecular envelopes of RV Tauri, red supergiants and Miras.

show abstract

Limb-darkening corrections for interferometric uniform disc stellar angular diameters

Cited by 77 publications

References 13 publications

Spherically-symmetric model stellar atmospheres and limb darkening

Spherically-symmetric model stellar atmospheres and limb darkening

Interferometric properties of pulsating C-rich AGB stars

Extended envelopes around Galactic Cepheids

Contact Info

Product

Resources

About