Sentences with phrase «high mass star»

μm) spectra, obtained on the 2.7 m Harlan J. Smith Telescope at McDonald Observatory with the Immersion Grating INfrared Spectrometer (IGRINS)(Park et al. 2014, SPIE, 9147, 1), for a variety of Galactic PDRs including regions of high mass star formation, reflection nebulae, and planetary nebulae.

In the center of the image the young high mass star appears as a small and weak red spot.

I am particularly interested in environmental effects on star and planet formation, such as in high mass star forming regions, where external photoevaporation may play an important role on disk evolution and planet formation.

After shining for many millions of years, stars end their lives, mainly, in two ways: very high mass stars die very violently as supernovae, while low mass stars end as planetary nebulae.

Although higher mass stars are rarer than lower mass ones, astronomers had expected to find three or four of them with masses between 18 and 30 times the mass of the Sun.

This is why previous theories have suggested that the model of a small star forming from a protoplanetary gas and dust disk isn't applicable to high mass stars.

For higher mass stars with up to 10 solar masses, the hydrogen surrounding the helium core reaches sufficient temperature and pressure to undergo fusion, forming a hydrogen - burning shell.

Not exact matches

If black hole after all the scenario of quantum mechanical process have completed their interactions behave accordingly to Relativity equation to became eventually a tiny speck in space of high intensity mass with very strong gravitation wave could the telescope have picked up such polarization of light from some gravitated wave of dying star or black hole.

Chris Evans, the principal investigator of VFTS and a co-author of the study, said: «In fact, our results suggest that most of the stellar mass is actually no longer in low - mass stars, but a significant fraction is in high - mass stars.»

This large sample allowed the scientists to derive the most accurate high - mass segment of the IMF to date, and to show that massive stars are much more abundant than previously thought.

2 According to Turnbull, stars must be at least 3 billion years old (to allow life time to evolve), have low mass, and have high levels of iron; metals are needed to form rocky, Earthlike planets.

The extra material the higher - mass stars hold onto could then fall into the black holes, bulking them up.

That means lower - mass stars that go on to form neutron stars would blast more of their outer layers away than higher - mass stars that become black holes.

This object is one of the closest stellar nurseries for both low and high - mass stars, at a distance of about 1350 light - years [1].

Current observatories could also help reveal what makes spinning neutron stars called pulsars tick, mapping their starquake - shaken interiors and any centimeters - high «mountains» (which would weigh roughly the mass of a planet because of neutron stars» extreme density) that could pop up on their surfaces.

«We conducted radio observations of carbon monoxide and methanol to explore the details of the distribution and kinematics of gas in the region where high - mass stars are forming in clusters,» Higuchi said.

«A typical example of a high - mass star forming region is the Orion Nebula, but ALMA enabled us to see the complex formation environment of star clusters which is even 7 times farther away than the Orion Nebula with the highest imaging resolution ever achieved.

Since it is thought that high - mass stars are born in clusters far away from the Earth, it is impossible to understand their formation process in detail without high angular resolution observations.

Another adverse condition in the study of high - mass stars is the distance from the Earth; while the forming regions of low - mass stars are about 500 light years away from the Earth, those of high - mass stars are farther and even the closest one in the Orion Nebula is about 1500 light years away.

Detailed observations of high - mass stars have been considered difficult so far because high - mass stars form in a complex environment with multiple protostars in clusters, and their forming regions are located farther away from the Earth compared to those of low - mass stars.

«Even though many of the astronomers assumed that this would be a fertile high - mass star forming region, we couldn't probe the kinematics of gas around high - mass protostars at the level of resolution provided by existing telescopes,» Higuchi said.

It is the first time that such an hourglass structure was found in observations of methanol in high - mass star forming regions.

The formation process of high - mass stars which have masses larger than 10 times solar mass still has much to be explored.

It is thought that these gas clouds are surrounding a newly forming high - mass star like a cocoon.

An international team of astronomers has identified a record breaking brown dwarf (a star too small for nuclear fusion) with the «purest» composition and the highest mass yet known.

Lighter colors represent higher densities, marking the locations of two developing low - mass stars.

In the case of disk instability, ice giants form when the star system is located in the region of high - mass star formation.

«Not only does this star have the high velocity expected if it is recoiling from a supernova explosion, but the combination of its low mass, high luminosity and carbon - rich composition appear impossible to replicate in a single star — a smoking gun that shows it must have originally formed with a binary companion,» adds Ben Ritchie (Open University), a co-author on the new paper.

In addition, HESS has detected emissions from new classes of objects emitting very high energy gamma rays, such as stellar - mass black holes orbiting massive stars, and has characterized the absence of emissions from other classes of objects such as rapidly moving stars.

This finding is counterintuitive because higher - mass stars flood their planetary systems with energetic ultraviolet radiation that should destroy the carbon monoxide gas lingering in their debris disks.

More important, high - mass clusters produce high - mass stars — brightly burning nuclear furnaces 10 to 100 times the mass of our sun.

In low - mass clusters, feedback from the jets may play the same disruptive role as do winds and UV radiation from big stars in high - mass clusters.

The havoc of star - formation feedback is not confined to high - mass clusters.

In the high - mass kind, like the great Orion nebula, which is about 1,500 light - years away, stars are packed together like a swarm of bees.

Unfortunately, we do not yet have enough information to say whether most stars in the galaxy were formed in high - mass or low - mass clusters.

The tendency of very massive galaxies to contain a high fraction of low - mass stars at their centers is a recent discovery, and is still in some ways controversial, but is reinforced by the work reported here.

This means that this region will have a higher fraction of low - mass stars than in other zones of the galaxy.

That star is between 10 and 20 times the mass of our sun, and it's churning out a powerful wind of high - energy particles.

Such stars have masses of at least eight times that of the Sun and high surface temperatures of 10 000 K or more, but they exhaust their hydrogen supply more quickly than starts of lower mass: over some tens of mil - lions of years, compared to billions of years for stars like the Sun.

The best estimates for the occurrence rates of habitable zone earth - sized planets around sun - like stars is about 50 %, and for lower - mass stars this value is likely to be even higher: most red dwarf stars are expected to have one or more habitable zone, approximately earth - sized planets.

A second mode provides low spectral resolution but high sensitivity and is popular for studies of distant galaxies and very cool low - mass stars.

Eventually, Stars Aa and Ab will lose much of their current mass, from intensified stellar winds that eventually puff out their outer gas envelopes of hydrogen and helium (and lesser amounts of higher elements such as carbon and oxygen) into interstellar space as planetary nebulae.

Star B, a orange - red dwarf with a relatively calm chromosphere and acoustic p - wave mode oscillations, is an easier target for detecting wobbles from terrestrial planets, possibly within only three years of «high cadence» observations for a 1.8 Earth - mass planet (more from New Scientist and Guedes et al, 2008).

Combining two results, gas jets and outflows have a crucial role in removing the rotational momentum both in low - mass and high - mass star formation processes..

[50][51] Stars with at least four solar masses can also fuse elements with higher atomic numbers.

Although they are relatively rare, high - mass stars are the brightest and hottest of all, and are best observed at the shorter, higher - energy wave - lengths of UV to visible blue light.

This discovery extends the observation of protoplanetary disks to the high mass regime, where the dynamic is dominated by the mass of the disk rather than the mass of the central star.

Star B, the chromospherically calmer, orange - red dwarf, is an easier target for detecting wobbles from terrestrial planets, possibly within only three years of «high cadence» observations for a 1.8 Earth - mass planet (more from New Scientist and Guedes et al, 2008).

During this time, high - mass stars produce powerful «winds» (streams of energetic particles) that can trigger or halt star formation in their surroundings.

Before the heavens were stretched out, those stars had high velocities, because they were near a galaxy's center of mass where a black hole was growing.