منابع مشابه
Periodic radial velocity variations in RU Lupi ⋆
Context. RU Lup is a Classical T Tauri star with unusually strong emission lines, which has been interpreted as manifestations of accretion. Recently, evidence has accumulated that this star might have a variable radial velocity. Aims. We intended to investigate in more detail the possible variability in radial velocity using a set of 68 high-resolution spectra taken at the VLT (UVES), the AAT ...
متن کامل3D velocity from 3D Doppler radial velocity
We present local least squares and regularization frameworks for computing 3D velocity (3D optical flow) from 3D radial velocity measured by a Doppler radar. We demonstrate the performance of our algorithms quantitatively on synthetic radial velocity data and qualitatively on real radial velocity data, obtained from the Doppler radar at Kurnell Radar station, Botany Bay, New South Wales, Austra...
متن کاملRadial Velocity Variations in K Giants: Planets or Pulsations?
Radial velocity observations of K giants have revealed periodic variations for some of the stars. The periods range from approximately 180 to 1000 or more days with velocity amplitudes ranging from approximately 50 m/s to 500 m/s. Except for Iota Draconis (Frink et al. 2002), all variations are nearly sinusoidal. Companions with zero orbital eccentricity as well as pulsations may cause these ra...
متن کاملRadial Velocity Variations in Pulsating Ap Stars . II . 33 Librae ⋆
We present precise relative radial velocity (RV) measurements for the rapidly oscillating Ap (roAp) star 33 Librae measured from high resolution data spanning the wavelength interval 5000–6200 Å. We find that pulsational radial velocity amplitude determined over a broad wavelength range (≈ 100 Å) depends on the spectral region that is examined and can be as high as 60 m s at 5600 Å and as low a...
متن کاملTidally induced radial-velocity variations in close binaries
A theoretical framework for the determination of tidally induced radial-velocity variations in a component of a close binary is presented. Both the free and the forced oscillations of the component are treated as linear, isentropic perturbations of a spherically symmetric star. Resonances between dynamic tides and free oscillation modes are taken into account by means of the formalism developed...
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ژورنال
عنوان ژورنال: International Astronomical Union Colloquium
سال: 1999
ISSN: 0252-9211
DOI: 10.1017/s0252921100048648