Sentences with phrase «stellar radial velocity»

Still, many of the nearby planets are detectable via three exoplanet hunting methods: planetary transits, high - contrast imaging, and stellar radial velocity measurements.

Not exact matches

Both 61 Vir b and HD 1461 b were detected by radial velocity, or stellar wobble, measurements alone, meaning that their diameters remain unknown.

«These data recover the well - known solar 5 - minute oscillation at a peak of 3 mHz (5.5 min) from the disk - averaged light with a radial - velocity amplitude of only 47 cm / s, an incredibly small velocity from a stellar point of view», says Prof. Strassmeier, PEPSI principal investigator and director of the Cosmic Magnetic Field branch at the Leibniz Institute for Astrophysics Potsdam (AIP).

As part of a large survey of possible planet - hosting stars, Lovis and his colleagues used the powerful HARPS (for High Accuracy Radial - Velocity Planet Searcher) spectrograph at La Silla Observatory in Chile, 2,400 meters above sea level, which can detect stellar motions with precisions of less than one meter per second, roughly the walking speed of a human being.

Due to the close binary orbital interactions of the host star with Alpha Centauri A and Star B's own increased stellar activity during recent years, the astronomers were only able to detect the radial - velocity variations of host star B that were caused by the 3.236 - day orbit of the planet (with a semi-major axis of 0.04 AU) only after more than four and a half years of careful observation.

In July 2008, astronomers (Michael Endl and Martin Kürster) analyzed used seven years of differential radial velocity measurements for Proxima Centauri to submit a paper indicating that large planets are unlikely to be orbiting Sol's closest stellar neighbor within its habitable zone — around 0.022 to 0.054 AU with a corresponding orbital period of 3.6 to 13.8 days.

Due to the close binary orbital interactions of the host star with Alpha Centauri A and Star B's own increased stellar activity during recent years, the astronomers were only able to detect the radial - velocity variations of host star B that were caused by the 3.236 - day orbit of the planet (with a semi-major axis of 0.04 AU) only after more than three years of careful observation.

Zeta1 has a brighter but distant stellar companion, Zeta2 Reticuli, currently located around 3,750 AUs away (based on an observed separation of 310» and HIPPARCOS distance estimates of 39.40 to 39.53 ly), with common proper motion and equal radial velocities (Da Silva and Foy, 1987).

In the EDEN / RV component we are utilizing stellar reflex motion (radial velocity measurements) to search for extrasolar planets around nearby stars.

Our barycentric radial velocities, derived from observations taken at the KPNO 2.1 meter telescope, differ from... ▽ More We demonstrate the ability to measure precise stellar barycentric radial velocities with the dispersed fixed - delay interferometer technique using the Exoplanet Tracker (ET), an instrument primarily designed for precision differential Doppler velocity measurements using this technique.

The distances of individual stars in a moving group may be determined if their radial velocities and proper motions are known (see below Stellar motions) and if the exact position of the radiant is determined.

In addition, Tau Ceti does not appear to have a close stellar or substellar companion based on astrometric measurements (Lippincott and Worth, 1980), radial velocity variations (Campbell et al, 1988; and near - infrared interferometry (Di Folco et al, 2007).

We combine this dataset with distance estimates... ▽ More Our long term aim is to derive model - independent stellar masses and distances for long period massive binaries by combining apparent astrometric orbit with double - lined radial velocity amplitudes (SB2).

Abstract: Our long term aim is to derive model - independent stellar masses and distances for long period massive binaries by combining apparent astrometric orbit with double - lined radial velocity amplitudes (SB2).

We first generate a stellar field with planetary companions based on radial velocity discoveries, use a planetary evolution model assuming a variable fraction of heavy elements to compute the characteristics of transit events, then apply a detection criterion that includes both statistical and red noise sources.