Sentences with phrase «radial velocity variations of»

[1] Most of the exoplanets currently known were discovered using indirect techniques — such as radial velocity variations of the host star, or the dip in brightness of the star caused by a transiting exoplanet.

Not exact matches

The planet was found with the radial velocity method, a planet - hunting technique that relies upon slight variations in the velocity of a star to determine the gravitational pull exerted by nearby planets that are too faint to observe directly with a telescope.

The radial - velocity variations indicate a highly eccentric orbit with a period of 153.9 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 four and a half years of careful observation.

I. Performances of radial velocity measurements, first analyses of variations.

On March 25, 2015, a team of astronomers using the Hubble Space Telescope revealed observations which indicate via the transit method that Alpha Centauri B may have a second planet «c» in a hot inner orbit, just outside planet candidate «b.» After observing Alpha Centauri B in 2013 and 2014 for a total of 40 hours, the team failed to detect any transits involving planet b (previously detected using the radial velocity variations method and recently determined not to be observed edge - on in a transit orbit around Star B).

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.

Prior to 2009, small but significant variations in radial velocity had been detected which may have been caused by a substellar companion of one to nine Jupiter - masses with an orbital period of 50 years of less (Campbell et al, 1988, pages 904, 906, and 919).

The transit signals were detected in photometric data from the Kepler satellite, and were confirmed to arise from planets using a combination of large transit - timing variations, radial - velocity variations, Warm - Spitzer observations, and statistical analysis of false - positive probabilities.

As a subgiant star subject to pulsations which affect careful measurements of variations in radial velocity caused by the gravitational pull of substellar companions, astronomers would find it very difficult to detect any Earth - type planet around Beta Hydri using present methods.

Kepler - 19 joins the small number of systems that reconcile transit timing variation and radial velocity measurements.

Kepler 18 - b, c, and d: A System Of Three Planets Confirmed by Transit Timing Variations, Lightcurve Validation, Spitzer Photometry and Radial Velocity Measurements

Radial velocity observations from observing runs in 2000 and 2004 reveal a periodic variation of 3.30 ± 0.02 d, which is consistent with the previously determined value of 3.3125 ± 0.0002 d.

If you are new to this saga make sure you read Tau II Abstract: The successful detection is reported of radial - velocity variations due to orbital motion of the substellar companion of the star tau Boötis, from data obtained with a small aperture (0.4 - m) telescope and a fibre - fed high resolution spectrograph.

The primary shows long - period radial velocity variations that indicate the presence of a low mass companion whose projected mass is in the planetary regime (m sin i = 9.33 Mjup).

However, the high luminosity of the primary star, intense Ca II H and K emission (Smith and Dominy, 1979), and radial velocity variations somewhat larger than can be accounted for by the expected uncertainties suggested that Delta Eridani might be an RS CVn - type binary and therefore a photometric variable like most members of that class.

Analysis of radial velocity variations suggest that this probable red dwarf star has about 15 percent of Sol's mass (Irwin et al, 1992).

As CORVAL monitoring failed to detect significant radial velocity variations over period of 3,400 days — or over 9.3 years (Duquennoy and Mayor, 1991, pp. 492 and 506), the detection is now considered to be spurious.

High - precision radial - velocity measurements confirm a sinusoidal variation with the period and phase predicted by the photometry, and rule out the presence of line - bisector variations that would indicate that the spectroscopic orbit is spurious.

We also find a slow variation in the radial velocity of Procyon, with good agreement between different telescopes.

Scientists were also able use the infrared spectroscopy to look at radial velocity variations (an analysis of the light spectrum) to determine that water was present.