Protostar contraction to the Main Sequence, like the pre-visible protostellar cloud contraction, is fairly rapid for large mass stars and fairly slow for lower mass stars As a result massive stars can go from the initial cloud collapse all the way to the Main Sequence in just a few 10's...
where all grains smaller than 0.1μm would have been removed in the parent cloud before the collapse. Conclusions.When grain drift velocities induced by ambipolar diffusion are included, dust coagulation happening during the collapse of a prestellar core starting from an initial MRN dust size ...
Here we present observations of four highly collimated jets from young stars that appear to have been stripped of their circumstellar molecular cloud cores in this way. The production of jets seemstohave been largely unaffected. If these jets are also photoionized, their mass loss rates can be...
Can a rocky planet form directly from the collapse of an interstellar gas cloud? The picture I have of rocky planet formation is that dust and rocky material in a protostellar disk accumulates into a rocky planet. There must be some mechanism to prevent the accretion of significant amounts of...
In this image of the Serpens Nebula from the Near-Infrared Camera (NIRCam) on NASA’s James Webb Space Telescope, astronomers found a grouping of aligned protostellar outflows within one small region (the top left corner). Serpens is a reflection nebula, which means it’s a cloud of gas...
start to form clumps. As these clumps accumulate more material, they grow in mass. Thanks to their own gravity, they pull in even more gas and dust from the surrounding star-forming region. Over a million years (give or take), these clumps mature into dense bodies known as protostars. ...
(NIRCam). In this image, throughout the region, filaments and wisps of different hues represent reflected starlight from still-forming protostars within the cloud. In some areas, there is dust in front of that reflection, which appears here with an orange, diffuse shade. C...
One of the most fascinating aspects of stellar formation is the enormously vast change of physical parameters during the process of gravitational cloud collapse. A comparison of the initial density in a molecular cloud core with the average density in mature stars, for example, reveals a difference...
Based on the census of prestellar cores, Class 0 protostars, and more evolved YSOs, we conclude that the star formation rate has decreased with time in this cloud. The low fraction of candidate prestellar cores among the population of starless cores, the small number of Class 0 protostars...
F. Disk masses in the Orion Molecular Cloud-2: distinguishing time and environment. Astron. Astrophys. 628, A85 (2019). Article CAS Google Scholar Clarke, C. J. & Pringle, J. E. Accretion disc response to a stellar fly-by. Mon. Not. R. Astron. Soc. 261, 190–202 (1993). ...