Results 251 to 260 of about 4,471,573 (294)
Some of the next articles are maybe not open access.
Nature Climate Change, 2020
Gravity-based estimates of mass change have been extended by the recently launched GRACE Follow-On Satellites. The satellite record, combined with regional climate models, reveals that the Greenland Ice Sheet had lower mass loss in 2017–2018, only to return to a record-breaking mass loss in the summer of 2019.
openaire +2 more sources
Gravity-based estimates of mass change have been extended by the recently launched GRACE Follow-On Satellites. The satellite record, combined with regional climate models, reveals that the Greenland Ice Sheet had lower mass loss in 2017–2018, only to return to a record-breaking mass loss in the summer of 2019.
openaire +2 more sources
1978
The decrease of total mass by ejection past the outer Lagrangian points is a distinct possibility, probably a necessity, in the explanation of late phases of evolution, and some instances have been mentioned earlier. One indication noted by van den Heuvel (1969) may apply to a large fraction of the binary population, namely that much fewer semi ...
openaire +1 more source
The decrease of total mass by ejection past the outer Lagrangian points is a distinct possibility, probably a necessity, in the explanation of late phases of evolution, and some instances have been mentioned earlier. One indication noted by van den Heuvel (1969) may apply to a large fraction of the binary population, namely that much fewer semi ...
openaire +1 more source
2001
The problem of mass loss is described in the context of non-linear radial pulsations of luminous stars. The numerical requirements of such computations are briefly discussed. The first example is devoted to models of dust-driven winds from AGB-stars. The second part illustrates numerical computations of LBVs in some detail to understand the long term ...
Ernst A. Dorfi +2 more
openaire +1 more source
The problem of mass loss is described in the context of non-linear radial pulsations of luminous stars. The numerical requirements of such computations are briefly discussed. The first example is devoted to models of dust-driven winds from AGB-stars. The second part illustrates numerical computations of LBVs in some detail to understand the long term ...
Ernst A. Dorfi +2 more
openaire +1 more source
EAS Publications Series, 2013
Betelgeuse is just starting to produce a wind which is thick enough to form dust. However, the grains seem to coalesce at much greater distances than those in “dust-driven” winds from later-stage AGB and RSG stars. Is the mass loss mechanism different, and how will it evolve?
openaire +1 more source
Betelgeuse is just starting to produce a wind which is thick enough to form dust. However, the grains seem to coalesce at much greater distances than those in “dust-driven” winds from later-stage AGB and RSG stars. Is the mass loss mechanism different, and how will it evolve?
openaire +1 more source
Astrophysics and Space Science, 1979
The evolution of spin in a star undergoing adiabatic mass loss is considered. It is established that adiabatic mass loss cannot drive spin. If such a mass loss is due to a binary component overflowing its Roche lobe then this result rules out the possibility of asynchronous rotation in close contact systems.
openaire +1 more source
The evolution of spin in a star undergoing adiabatic mass loss is considered. It is established that adiabatic mass loss cannot drive spin. If such a mass loss is due to a binary component overflowing its Roche lobe then this result rules out the possibility of asynchronous rotation in close contact systems.
openaire +1 more source
Science, 2018
Ice Sheets The Greenland Ice Sheet, along with the Antarctic Ice Sheet and glaciers worldwide, is melting at an accelerating rate. This melting is not uniform, however, with adjacent fjords often exhibiting quite different behaviors. What can account for those differences? Millan et al.
openaire +1 more source
Ice Sheets The Greenland Ice Sheet, along with the Antarctic Ice Sheet and glaciers worldwide, is melting at an accelerating rate. This melting is not uniform, however, with adjacent fjords often exhibiting quite different behaviors. What can account for those differences? Millan et al.
openaire +1 more source
Publications of the Astronomical Society of Australia, 1977
The visual spectra of some hot stars, including P Cygni, have emission with associated absorption troughs ˜ 102 km s-1 on the short-wavelength side (Beals 1929, 1951). These P Cygni profiles are easily understood in terms of mass flowing away from the star.
openaire +1 more source
The visual spectra of some hot stars, including P Cygni, have emission with associated absorption troughs ˜ 102 km s-1 on the short-wavelength side (Beals 1929, 1951). These P Cygni profiles are easily understood in terms of mass flowing away from the star.
openaire +1 more source
Is Weight Loss–Induced Muscle Mass Loss Clinically Relevant?
JAMAThis Viewpoint explores the effects of weight loss achieved through GLP-1–based antiobesity medications on weight regain, fat-free mass, and skeletal muscle mass in people with obesity.
Caterina, Conte +2 more
openaire +2 more sources
Mira Light Curves and Mass Loss
Astrophysics and Space Science, 1994Long Period Variables represent a late stage in the evolution of intermediate mass stars. Mass loss wich leads them to planetary nebulae within a few 105 years, is a complex process and the object of many investigations. Recents studies suggest that mass loss could occur in brief superwind phases separated by long quiescent periods.
openaire +1 more source
2001
Stars return mass to the interstellar medium throughout their lives. A low-luminosity star such as the Sun is losing mass by a stellar wind at a rate of 10-14 solar masses per year (M ⊙yr-1). Very luminous stars, whether they are early-type hot stars or cool giants, lose mass at a rate of up to about 10-5 M ⊙yr- 1, and such rates have major ...
openaire +1 more source
Stars return mass to the interstellar medium throughout their lives. A low-luminosity star such as the Sun is losing mass by a stellar wind at a rate of 10-14 solar masses per year (M ⊙yr-1). Very luminous stars, whether they are early-type hot stars or cool giants, lose mass at a rate of up to about 10-5 M ⊙yr- 1, and such rates have major ...
openaire +1 more source