Sentences with phrase «of planetary companions»
Due in part of discoveries of planetary companions around this Sun - like star, 47 Ursae Majoris became one of the top 100 target stars for NASA's proposed Terrestrial Planet Finder (TPF), which is now indefinitely delayed.
http://members.nova.org/
Due in part to the discovery of planetary companions, Upsilon Andromedae A was identified as one of the top 100 target stars for NASA's proposed Terrestrial Planet Finder (TPF).
On January 16, 2002, a team of astronomers (including (Debra A. Fischer, Geoffrey W. Marcy, R. Paul Butler, Steven S. Vogt, and Gregory W. Henry) announced the discovery of a planetary companion «b,» whose mass has been estimated at a minimum of 20 percent that of Jupiter (exoplanets.org; and Fischer et al, 2003, in pdf) with a similar diameter.
Not exact matches
For those who prefer a more macho approach, planetary scientist Steven Chesley of NASA's Jet Propulsion Laboratory has proposed a companion mission called ISIS.
An intensive spectrographic search for companions of 123 comparatively nearby stars provides a clue to the frequency of such planetary systems
In this two - hour PBS special (a fine companion to The Life of Super-Earths), NOVA combines cutting - edge planetary science with the thrill of human exploration, putting astronomers and astrobiologists «on location» across the solar system as they explain the scientific search for life on other worlds.
The low luminosity of the companions and the estimated age of the system imply planetary masses between 5 and 13 times that of Jupiter.
Astronomers detect planets by spotting stars that repeatedly wobble toward and away from Earth, tugged by the gravity of one or more planetary companions.
The leading hypothesis for the moon's formation contends that a massive impact billions of years ago knocked a wealth of planetary material off of Earth, which coalesced into our lunar companion.
However, the inner, eccentric orbit of a giant planetary companion «b» recently discovered around 54 Piscium would probably disturb the orbit of such an Earth - type planet.
A planetary companion around the foreground star can produce a variation in the brightening of the background star.
We conclude that the planetary scenario is more likely than that of an astrophysical false positive by a factor of 2e5 (Kepler - 20b), 1e5 (Kepler - 20c), and 1.1 e3 (Kepler - 20d), sufficient to validate these objects as planetary companions.
We confirmed the planetary nature of the transiting companion using this mass limit and Doppler tomographic observations to verify that the companion transits HD 332124.
We identified the initial transit signal in the KELT - North survey data and established the planetary nature of the companion through precise follow - up photometry, high - resolution spectroscopy, precise radial velocity measurements, and high - resolution adaptive optics imaging.
We confirmed the planetary nature of the transiting companion using this mass limit and Doppler tom... ▽ More We present the discovery of KELT - 21b, a hot Jupiter transiting the $ V = 10.5 $ A8V star HD 332124.
Archival and follow - up photometry, the Gaia parallax, radial velocities, Doppler tomography, and adaptive optics imaging were used to confirm the planetary nature of the companion and characterize the system.
Following the announcement of the discovery of Proxima b, the Red Dots campaign aims at detecting additional small planetary sized companions to Proxima Centauri.
Orbital stability provides upper limits for the masses of the transiting companions that are in the planetary regime.
The observations suggest that the dust was created by collisions in a Edgeworth - Kuiper - like belt of icy bodies, and that the orbital asymmetry could be an indication that the dust is being shepherded by an unseen planetary companion — among other explanations (Eiroa et al, 2010).
Abstract: In recent years there have been many attempts to characterize the occurrence of stellar, BD and planetary - mass companions to solar - type stars, with the aim of constraining formation mechanisms.
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).
Assuming that the spectroscopic companion B does not preclude a stable inner planetary orbit, the distance from Star A where an Earth - type planet would be «comfortable» with liquid water is centered around only 0.457 AU — between the orbital distances of Mercury and Venus in the Solar System.
Detailed modeling of the transit is consistent with a planetary companion with an orbital period of 3.548460 + / -0.000032 days and a radius of 1.431 + / -0.050 Rj.
On June 24, 2009, astronomers submitted a paper summarizing observations which reveals that Star A reverses its magnetic poles every two years (some 11 times faster than our Sun, Sol), possibly because of the close orbit of its Jupiter - class planetary companion (Fares et al, 2009; and Unknown, New Scientist, July 13, 2009).
On the other hand, the discovery of a brown dwarf companion in a wide orbit that could perturb dormant comets in an Oort Cloud around Epsilon Indi inwards towards the star's inner planetary regions may periodically shower an Earth - type, inner planet with catastrophic impacts.
We detected the transit light - curve signature in the course of the TrES multi-site transiting planet survey, and confirmed the planetary nature of the companion via multicolor photometry and precise radial velocity measurements.
The dilution of the host star's light by the nearly equal magnitude stellar companion (~ 0.5 magnitudes fainter) significantly affects the derived planetary parameters, and if left uncorrected, leads to an underestimate of the radius and mass of the planet by 10 % and 60 %, respectively.
The dilution of the host star's light by the nearly equal magnitude stellar companion (~ 0.5 magnitudes fainter) significantly affects the derived planetary parameters, and if left uncorrected, leads to an underestimate of the radius and mass of the planet by 10 %... ▽ More We present the discovery of a hot Jupiter transiting an F star in a close visual (0.3» sky projected angular separation) binary system.
However, if the existence of a relatively close, second companion (see Star Bc below) around Bab — with an orbital period of 2.2 to 2.9 years or less — is confirmed, then a planetary orbit in Star Ba's water zone may not be stable over the long run.
After analyzing four years of Kepler space telescope observations, astronomers from the University of Toronto, and of the University of Cambridge have given us our clearest understanding yet of a class of exoplanets called «warm Jupiters», showing that many have unexpected planetary companions.
The finding of a 3.3 - day stellar rotation period for Star A that is estimated to be very similar to that of its recently discovered planetary companion moving in a very close «torch» orbit suggests that the planetary object may have tidally locked the star (Brogi et al, 2012; and Butler et al, 1997).
On September 24, 2002, a team of astronomers (including William D. Cochran, Artie P. Hatzes, Michael Endl, Diane B. Paulson, Gordon A. H. Walker, Barbara McArthur, Bruce Campbell, and Stephenson Yang) at the Planetary Systems and their Formation Workshop announced the preliminary confirmation of a long - suspected planetary companion «A1» (or «b») with a minimum mass of 1.76 that of Jupiter (MacDonald Observatory's Gamma Cephei and press release; Tautenburg Observatory press release in German; DPS session summary; Walker et al, 1992; Lawton and Wright, 1989; and Campbell et al, 1988), with a similar Planetary Systems and their Formation Workshop announced the preliminary confirmation of a long - suspected planetary companion «A1» (or «b») with a minimum mass of 1.76 that of Jupiter (MacDonald Observatory's Gamma Cephei and press release; Tautenburg Observatory press release in German; DPS session summary; Walker et al, 1992; Lawton and Wright, 1989; and Campbell et al, 1988), with a similar planetary companion «A1» (or «b») with a minimum mass of 1.76 that of Jupiter (MacDonald Observatory's Gamma Cephei and press release; Tautenburg Observatory press release in German; DPS session summary; Walker et al, 1992; Lawton and Wright, 1989; and Campbell et al, 1988), with a similar diameter.
However, the giant planetary companion «A1» or «b» recently discovered around Star A could disturb the stability or the development of such a rocky planet in this orbit.
On September 24, 2002, astronomers at the Planetary Systems and their Formation Workshop announced the preliminary confirmation of a long - suspected, Jupiter - type planetary companion within two AUs of Gamma Cephei A (see: MacDonald Observatory's Gamma Cephei and press release; Tautenburg Observatory in German; DPS session summary; Walker et al, 1992; Lawton and Wright, 1989; and Campbell et al, 1988 — more detailPlanetary Systems and their Formation Workshop announced the preliminary confirmation of a long - suspected, Jupiter - type planetary companion within two AUs of Gamma Cephei A (see: MacDonald Observatory's Gamma Cephei and press release; Tautenburg Observatory in German; DPS session summary; Walker et al, 1992; Lawton and Wright, 1989; and Campbell et al, 1988 — more detailplanetary companion within two AUs of Gamma Cephei A (see: MacDonald Observatory's Gamma Cephei and press release; Tautenburg Observatory in German; DPS session summary; Walker et al, 1992; Lawton and Wright, 1989; and Campbell et al, 1988 — more details below).
Observations of such eccentric structures provide potential evidence of the presence of such a companion in a planetary system.
No hints for the presence of an additional planetary companion in the two systems were found either from the photometric or radial velocity measurements.
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.
Researchers using data from Hubble's now - retired Wide Field Planetary Camera 2 (WFPC2) have identified two types of blue stragglers in Messier 30: those that form in near head - on collisions with one another and those that are in twin (or binary) systems where the less massive star siphons «life - giving» hydrogen from its more massive companion.
Gore's sobering view of global warming Former Vice President Al Gore's latest treatise on global warming, An Inconvenient Truth: The Planetary Emergency of Global Warming and What We Can Do About It , is a companion volume to the well - received documentary.