Sentences with phrase «planetary companions»

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.

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.

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.

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

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.

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).

Astronomers detect planets by spotting stars that repeatedly wobble toward and away from Earth, tugged by the gravity of one or more planetary companions.

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.

Scientists have long suspected that our planetary companion was built when a Mars - sized body — commonly known as Theia — struck the young Earth, throwing molten rock into orbit that coalesced into the Moon.

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.

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.

However, it may have emplaced the transiting planetary companion via the Kozai - Lidov mechanism.

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).

Forty precision Doppler measurements were used to confirm that the short - period transit event is due to a planetary companion.

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).

David Aguilar, Harvard - Smithsonian Center for Astrophysics — larger «day» and «night» images At maximum brightness, Mira would light up a hypothetical planetary companion, but at its most dark, the giant star's small, hot white dwarf companion would become visible (more discussion with illustration).

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 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 details below).

No hints for the presence of an additional planetary companion in the two systems were found either from the photometric or radial velocity measurements.

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.

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.

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.

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.

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.

No planetary or brown dwarf companions have been founded as yet (Lagrange et al, 2009).

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.

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.

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.

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.

H. Bond (STSci), R. Ciardullo (PSU), WFPC2, HST, NASA — larger image (Gacrux may have a white dwarf companion B, a remnant stellar core that has already cast off its outer gas layers, like planetary nebula NGC 2440.)

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.

H. Bond (STSci), R. Ciardullo (PSU), WFPC2, HST, NASA HD 147513 B is a young white dwarf (a remnant stellar core which enriched its binary companion, Star A) with elements heavier than hydrogen when it cast off its outer gas layers) like planetary nebula NGC 2440.

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.

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).

Observations of such eccentric structures provide potential evidence of the presence of such a companion in a planetary system.