Sentences with phrase «radial velocity analysis»

Past radial velocity analysis suggests that giant planets of one tenth to 10 times the mass of Jupiter do not exist within 0.1 to four AUs of 15 Sge (Cummings et al, 1999).

Subsequent studies failed to resolve a companion star, both by speckle interferometry (Hartkopf and McAlister, 1983) and by radial velocity analysis (Marcy and Benitz, 1989).

Past radial velocity analysis suggests that giant planets of one tenth to 10 times the mass of Jupiter do not exist within 0.1 to four AUs of Star A (Cummings et al, 1999).

Subsequently, more recent radial velocity analysis also failed to find supporting evidence (Young et al, 1987, page 5) for such an object.

Past radial velocity analysis suggests that giant planets of one tenth to 10 times the mass of Jupiter do not exist within 0.1 to four AUs of 37 Gem (Cummings et al, 1999).

[106] Theoretical studies on the detectability via radial velocity analysis have shown that a dedicated campaign of high - cadence observations with a 1 - meter class telescope can reliably detect a hypothetical planet of 1.8 M ⊕ in the habitable zone of B within three years.

The radial velocity analysis presented in this paper serves as example of the type of analysis that will be necessary to confirm the masses of TESS small planet candidates.

The two stars have a highly elliptical orbit, which radial velocity analyses suggest is 0.53 rather than 0.61 (Griffin, 1998).

The two stars have a highly elliptical orbit, and more recent radial velocity analyses suggest that the eccentricity is closer to 0.53, rather than the 0.61 value derived from visual observations (Griffin, 1998).

Not exact matches

A subsequent analysis using the most recent kinematic and radial velocity data available in the literature, however, found Proxima «is quitely likely» to be bound to to Stars A and B based on calculations of the binding energy of Proxima relative to the center of mass of the entire triple system, where its orbital semi-major axis exceeds 10,000 AUs and is «on order the same size as Alpha Centauri AB's Hill radius in the galactic potential» (Wertheimer and Laughlin, 2006).

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

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.

Here we present results from the analysis of 82 new radial velocity observations of this system obtained with HARPS - N, together with the existing 14 HIRES data points.

We present new mass measurements of three of the planets in the Kepler - 20 system facilitated by 104 radial velocity measurements from the HARPS - N spectrograph and 30 archival Keck / HIRES observations, as well as an updated photometric analysis of the Kepler data and an asteroseismic analysis of the host star (MStar = 0.948 + -0.051 Msun and Rstar = 0.964 + -0.018 Rsun).

Planet «d» or «3» - Planetary candidate d (or 3) was derived by Bayesian analysis of 47 UMa's radial velocity data.

Spectroscopic, astrometric and radial - velocity analyses reveal a companion with an average separation of 6.4 AUs (a semi-major axis derived from a photocentric estimate of 0.0969» times [1 + (mass A of 1.00 / mass B of 0.15)-RSB--- and a HIPPARCOS parallax of 0.11543 + / - 0.00108»), varying between 3.5 and 9.3 AUs.

In addition to precise differential velocities, this survey will also yield precise barycentric radial velocities for many thousands of stars using the data analysis techniques reported here.

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

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.

On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed two super-Earths «b» and «c» with minimum earth - masses of 4.4 (+3.7 / -2.4) and 8.7 (+5.8 / -4.7), respectively, at average orbital distances of 0.080 (+0.014 / -0.004) and 0.176 (+0.009 / -0.030) AU, respectively, from host star Gl 682, with orbital eccentricities of 0.08 (+0.19 / -.08) and 0.010 (+0.19 / -0.10) and periods around 17.5 and 57.3 days, respectively (UH news release; and Tuomi et al, 2014).

On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed two super-Earths «b» and «c.» Planet b has around 4.4 (+3.7 / -2.4) Earth - masses and an average orbital distance of 0.080 (+0.014 / -0.004) AU from host star Gl 682.

On March 4, 2014, a team of astronomers announced that analysis of new and older radial - velocity data from nearby red dwarf stars revealed a planet with a minimum of 32 (max 49) Earth - masses at an average orbital distance of 0.97 AU from host star Gl 229, with an orbital period around 471 days (UH news release; and Tuomi et al, 2014).