Physics
Scientific paper
Apr 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..apr..i801m&link_type=abstract
American Physical Society, APS/AAPT Joint April Meeting, April 18-21, 1998 Columbus, Ohio, abstract #I8.01
Physics
Scientific paper
The observed angular momentum (per unit mass) of a blob of interstellar matter destined to collapse and form stars is typically two to five orders of magnitude greater than that of single or binary stars. Hence, centrifugal forces would prevent the formation of stars if angular momentum were to be conserved during the contraction of a protostellar fragment. Further observational evidence reveals that this excess angular momentum is not stored in the orbital motions of stars in stellar clusters. It must get transported to the surrounding interstellar matter by some mechanism if stars of any kind are to form. We summarize the relevant observations and review the theoretical calculations, both analytical and numerical, which show that magnetic braking can and does resolve this thorny angular momentum problem of star formation. Magnetic braking first operates under physical conditions well approximated by ideal MHD and, subsequently, under conditions described by nonideal, multifluid MHD. Aside from explaining existing observations, the theoretical calculations predict observable physical quantities, such as the density, magnetic field and angular velocity structure in protostellar fragments and their vicinity. The general conclusion follows that stars (and solar systems) owe their very existence to cosmic magnetic fields.
No associations
LandOfFree
Angular Momentum Transport During Star Formation does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Angular Momentum Transport During Star Formation, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Angular Momentum Transport During Star Formation will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1603063