Sentences with phrase «brown dwarf companions in»

Epsilon Indi is an orange - red dwarf star, with two methane brown dwarf companions in orbit around each other (more).

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.

The orbit of an Earth - like planet around the tight binary system that star Ba forms with its brown dwarf companion in the liquid water zone would have to be centered around 1.1 AU — a little farther than Earth's orbital distance around Sol — with an orbital period exceeding one Earth year.

Not exact matches

Close encounter Tracing the trajectory of the star and its brown dwarf companion back in time, Mamajek's team found with 98 % confidence that Scholz's star passed within the Solar System's Oort cloud, a reservoir of comets, about 70,000 years ago.

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.

«Right now, the star and the brown dwarf are locked in a honeymoon phase, where they both turn the same face to each other all the time,» says Beatty, «but in the future, the star will swell up and engulf its companion completely.»

However, in a star - brown dwarf binary, the star's rotation is much slower than the brown dwarf's orbital motion, so the companion is dragged inward.

«Our knowledge of binary evolution suggests that, if the companion star can survive the transition, brown dwarfs should be common in this type of system.

In 1996, another group of astronomers using the Hubble Space Telescope discovered that they might have directly observed a companion to Proxima with the implied brightness of a brown dwarf and an apparent visual separation of only about half the Earth - Sun distance — 0.5 AU (Schultz et al, 1998).

Finally, we analyze the sensitivity of our data to additional closer - in companions and reject the possibility of other massive brown dwarf companions down to 4 - 5 AU.

We used NaCo at VLT to explore t... ▽ More In anticipation of the VLT / SPHERE planet imager guaranteed time programs, we have conducted a preparatory survey of 86 stars between 2009 and 2013 in order to identify new faint comoving companions to ultimately carry out a comprehensive analysis of the occurence of giant planets and brown dwarf companions at wide (10 - 2000 AU) orbits around young, solar - type starIn anticipation of the VLT / SPHERE planet imager guaranteed time programs, we have conducted a preparatory survey of 86 stars between 2009 and 2013 in order to identify new faint comoving companions to ultimately carry out a comprehensive analysis of the occurence of giant planets and brown dwarf companions at wide (10 - 2000 AU) orbits around young, solar - type starin order to identify new faint comoving companions to ultimately carry out a comprehensive analysis of the occurence of giant planets and brown dwarf companions at wide (10 - 2000 AU) orbits around young, solar - type stars.

We present new high - contrast data obtained during the commissioning of the SPHERE instrument at... ▽ More GJ758 B is a brown dwarf companion to a nearby (15.76 pc) solar - type, metal - rich (M / H = +0.2 dex) main - sequence star (G9V) that was discovered with Subaru / HiCIAO in 2009.

Abstract: GJ758 B is a brown dwarf companion to a nearby (15.76 pc) solar - type, metal - rich (M / H = +0.2 dex) main - sequence star (G9V) that was discovered with Subaru / HiCIAO in 2009.

Using the radial velocity technique pioneered by Geoffrey Marcy and Paul Butler, the Lick Planet Search for substellar companions has thus far failed to find a brown dwarf or large Jupiter - or Saturn - mass object in a «torch» orbit around Beta Comae Berenices (Cumming et al, 1999).

Using the radial velocity technique pioneered by Geoffrey Marcy and Paul Butler, the Lick Planet Search for substellar companions has thus far failed to find a brown dwarf or large Jupiter - or Saturn - mass object in a «torch» orbit around Chi1 Orionis A (Cumming et al, 1999).

In 2010, a new study (which included better model atmosphere fitting) argued that the system is around six billion years old, even older than estimates of 3.7 to 4.3 billion years derived from a 2009 study based on mass and evolutionary models for the two brown dwarf companions Ba and Bb (Liu et al, 2010; and King et al, 2009), which are much older than an earlier age estimate of between 0.8 and 2.0 billion years based on the star's rotational speed (press release; Scholz et al, 2003; and Lachaume et al, 1999).

Methane, carbon monoxide, and water molecules were detected in the relatively cool atmosphere of the brown dwarf companion (more).

Abstract: In this paper we present the results of the SPHERE observation of the HD 284149 system, aimed at a more detailed characterisation of both the primary and its brown dwarf companion.

As a result of this study, HD 284149 ABb therefore becomes the latest addition to the (short) list of brown dwarfs on wide circumbinary orbits, providing new evidence to support recent claims that object in such configuration occur with a similar frequency to wide companions to single stars.

Epsilon Indi ba is so cool that methane has been detected in its atmosphere and so it has been classified as the earliest T - type (T1 V), methane brown dwarf (McCaughrean et al, 2003)-- a «T - dwarf»), like the brown dwarf companion to Gliese 229.

In August 2003, the same team of astronomers as well as another team of astronomers (including Gordon Walker, Suzie Ramsay Howat, Kevin Volk, Robert Blum, David Balam, and Verne Smith) found that the brown dwarf had its own brown dwarf companion designated «bb» (Gemini press release and IAUC 8188).

The known brown dwarf companion (HD 284149 b) is clearly visible in the IRDIS images.

Using the radial velocity technique pioneered by Geoffrey W. Marcy and R. Paul Butler, the Lick Planet Search for substellar companions has thus far failed to find a brown dwarf or large Jupiter - or Saturn - mass object in a «torch» orbit around BD +04 123 (Cumming et al, 1999).

Moreover, the brown dwarf companion to 15 Sge may eventually prove to have a highly circular orbit that is coplanar with the circumstellar disk so that planets formed in inner orbits around the star.

In August 2003, the same team (as well as another team) of astronomers discovered that the brown dwarf had its own brown dwarf companion (Gemini press release — more below).

Using the radial velocity technique pioneered by Geoffrey Marcy and Paul Butler, the Lick Planet Search for substellar companions has thus far failed to find a brown dwarf or large Jupiter - or Saturn - mass object in a «torch» orbit around Kappa Ceti (Cumming et al, 1999).

On January 13, 2003, a team of astronomers (including Ralf - Dieter Scholz, Mark McCaughrean, Nicolas Lodieu, and Bjoern Kuhlbrodt) announced the discovery of a brown dwarf companion «b» — now re-designated «ba» — to this nearby star with a total (bolometric) luminosity of just 0.002 percent that of the Sun (ESO and AIP joint press release and API press release in German — more below).

On January 13, 2003, astronomers announced the discovery of a methane brown dwarf companion to this nearby star (ESO and AIP joint press release and API press release in German — more below).

Star Ba may have a brown dwarf companion (see Bb below) in a «torch orbit,» with an average separation of 0.06 AU in a highly circular orbit (e = 0.00) whose period is completed within four days.