Sentences with phrase «orbital velocity of»

Kipping's exomoon detection involves discovering its gravitational pull on the orbital velocity of a planet host — which in turn, are often detected based on their gravitational pull around a star.

The measured orbital velocity of this ring allows the calculation of the mass of the two galaxies and any dark matter.

Fritz Zwicky used it for the first time to declare the observed phenomena consistent with dark matter observations as the rotational speeds of galaxies and orbital velocities of galaxies in clusters, gravitational lensing of background objects by galaxy clusters such as the Bullet cluster, and the temperature distribution of hot gas in galaxies and clusters of galaxies.

Traditionally, the only way to accurately determine the mass of these hungry monsters has been to gauge the orbital velocities of stars nearby.

Not exact matches

He started the series of tweets with the acknowledgment that «This is gonna sound crazy,» and then said, «SpaceX will try to bring rocket upper stage back from orbital velocity using a giant party balloon.»

Musk floated an idea for upper stage recovery in a series of tweets recently, saying his company would bring Falcon 9's upper stage «back from orbital velocity using a giant party balloon.»

After that feat, Musk took to Twitter to offer his own congratulations, also couched with comments about the relative difficulty of landing from orbital versus suborbital velocities.

God so commands all orbital velocities inwardly from the lowly atoms and even outwardly toward issues of all that is made celestially orbital... Our humanoid embodiments of orbital atoms are merely buildings structured just so to be inhabited by godly generations on a scalar dimension unequaled in the inward depths and breadths of spatial reciprocity...

He argued that a star could not exist under the conditions described by Schwarzschild because the material within it would have to reach orbital velocities equaling the speed of light.

This separation is essential for the study of gravity because the effect of gravitational radiation — the steady conversion of orbital velocity to gravitational waves as predicted by Einstein — is incredibly small and would have negligible impact on the orbit of the pulsar.

The high - velocity impact of a piece of dust or orbital debris generates plasma and an associated Radio Frequency emission.

«Being hit by a 1 - centimetre object at orbital velocity is the equivalent of exploding a hand grenade next to a satellite,» says Heiner Klinkrad, head of the space debris office at the European Space Agency in Darmstadt, Germany.

Due to the close binary orbital interactions of the host star with Alpha Centauri A and Star B's own increased stellar activity during recent years, the astronomers were only able to detect the radial - velocity variations of host star B that were caused by the 3.236 - day orbit of the planet (with a semi-major axis of 0.04 AU) only after more than four and a half years of careful observation.

Therefore, the radial velocity surveys only pick the lowest hanging fruit: Jupiters that have migrated close in to their star, and have orbital periods of literally only a few days.

In July 2008, astronomers (Michael Endl and Martin Kürster) analyzed used seven years of differential radial velocity measurements for Proxima Centauri to submit a paper indicating that large planets are unlikely to be orbiting Sol's closest stellar neighbor within its habitable zone — around 0.022 to 0.054 AU with a corresponding orbital period of 3.6 to 13.8 days.

Even though the radial velocity method can only give some rough measurements of an exoplanet's properties, like minimum mass and orbital period, it nevertheless allows astronomers to make some educated guesses regarding the planet's overall structure.

Measurements of Gl 105A's radial velocity over 12 years show a linear trend and slope which is consistent with these orbital constraints and a nearly face - on orbit.

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).

Due to the close binary orbital interactions of the host star with Alpha Centauri A and Star B's own increased stellar activity during recent years, the astronomers were only able to detect the radial - velocity variations of host star B that were caused by the 3.236 - day orbit of the planet (with a semi-major axis of 0.04 AU) only after more than three years of careful observation.

However, later observations by other astronomers using interferometric astrometry and recent radial velocity data found no evidence to support the existence of a companion greater than 0.8 Jupiter mass with an orbital period around Proxima Centauri of between one and about 2.7 years (Benedict et al, 1999).

Prior to 2009, small but significant variations in radial velocity had been detected which may have been caused by a substellar companion of one to nine Jupiter - masses with an orbital period of 50 years of less (Campbell et al, 1988, pages 904, 906, and 919).

The planet has an orbital period of 1.486 days, and radial velocity measurements from the Hobby - Eberly Telescope (HET) show a Doppler signal of 420 + / -15 m.s - 1.

In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT - 22A suggesting the presence of another relatively nearby body that is perhaps non-stellar.

Starting from the Earth's orbital speed of 30 kilometers per second (km / s), the change in velocity (delta - v) the spacecraft must make to enter into a Hohmann transfer orbit that passes near Mercury is large compared to other planetary missions.

We also used radial velocity measurements of the host star, spanning a time range of $ \ sim $ 30 yr, to constrain the companion's mass and orbital properties, as well as to probe the host star's spectral age indicators and general spectral energy distribution.

Planet «c» or «2» - A residual drift in the radial velocity data over several years suggest the presence of an even larger planet in an outer orbit, at about 3.73 AUs from 47 UMa (between the average orbital distances of Jupiter and the Main Asteroid Belt in the Solar System).

If you are new to this saga make sure you read Tau II Abstract: The successful detection is reported of radial - velocity variations due to orbital motion of the substellar companion of the star tau Boötis, from data obtained with a small aperture (0.4 - m) telescope and a fibre - fed high resolution spectrograph.

Radial velocity measurements of Alpha Centauri B with High Accuracy Radial Velocity Planet Searcher spectrograph ruled out planets of more than 4 M ⊕ to the distance of the habitable zone of the star (orbital period P = 20velocity measurements of Alpha Centauri B with High Accuracy Radial Velocity Planet Searcher spectrograph ruled out planets of more than 4 M ⊕ to the distance of the habitable zone of the star (orbital period P = 20Velocity Planet Searcher spectrograph ruled out planets of more than 4 M ⊕ to the distance of the habitable zone of the star (orbital period P = 200 days).

The star was once suspected of being older than Sol, because it does not rotate rapidly and exhibits moderately high U, V, W velocities in its galactic orbital motion (Ken Croswell, 1995, pp. 253 - 254).

In the case of Edasich, however, the high orbital eccentricity of its companion made its motion distinguishable from stellar pulsation as the cause of the observed velocity variations.

Subsequently, Heintz (1996, page 411) suggested that such a companion to Star Ba would have to have a mass of at least half Sol's to reach detectable brightness, and that, among other orbital requirements, Bc's period would have to be less than an Earth year in order to account for the absence of effects on Ba's radial velocities and positions.

Using multi-epoch optical and near - IR follow - up spectroscopy with FLAMES on the Very Large Telescope and ISIS on the William Herschel Telescope we obtain a full orbital solution and derive the fundamental parameters of both stars by modelling the light curve and radial velocity data.

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).

This «Gas Tail» would be lost constantly, perhaps «blown away» by the «Solar Wind» or just left behind due to alteration of the velocity vector from the Earth's orbital motion if not for Gravity AND the Dipole «plasma production».