Sentences with phrase «in planetary companions»

Not exact matches

If hot super-Earths start out rocky, perhaps it is because the worlds form later than their puffy mini-Neptune companions, when there's less gas left in the growing planetary system to build an atmosphere.

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.

In all, the team found 17 candidate brown dwarf companions to red dwarf stars, one brown dwarf pair, and one brown dwarf with a planetary companion.

That causes our planetary companion to pop out from the synestia, leaving it in orbit around the body that will keep cooling until it resembles Earth.

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.

A planetary companion around the foreground star can produce a variation in the brightening of the background star.

Through N - body calculations, I will show that if hot Jupiters migrated by Lidov - Kozai oscillations driven by external planetary perturbers, close - in super-Earth companions would have been perturbed onto their host stars.

Older worlds with planetary companions may be the place to find the most ancient life in the galaxy, according to a new study.

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.

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).

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.

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.

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 %... ▽ 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.

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.

Such «barium stars» may be binaries, where a more massive companion has already thrown off its outer gas envelopes as a planetary nebula in becoming a white dwarf (see HD 147513 AB).

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.

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.