Convective accretion disk model for the primordial solar nebula

Details Convective accretion disk model for the primordial solar nebula Convective accretion disk model for the primordial solar nebula

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...246..972l&link_type=abstract

Astrophysical Journal, Part 1, vol. 246, June 15, 1981, p. 972-984.

Astronomy and Astrophysics

Astrophysics

49

Convective Heat Transfer, Nebulae, Protostars, Solar Corona, Stellar Evolution, Stellar Mass Accretion, Cosmology, Gravitational Effects, Magnetohydrodynamic Flow, Optical Thickness, Protoplanets, Solar System, Stellar Mass, Stellar Models

Scientific paper

Analytic steady-state solutions are presented for a self-consistent convective accretion disk model. These results are used to study the structure of the primordial solar nebula during the stage of protoplanetary formation. Arguments are presented in favor of protoplanetary formation by accretion rather than gravitational instability. Various dynamical constraints are used to provide quantitative estimates of the mass flux and viscosity of the nebula. Finally, the mass of the nebula and the time available for protoplanetary growth are estimated.

Affiliated with

Also associated with

No associations

Rating

Convective accretion disk model for the primordial solar nebula 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 Convective accretion disk model for the primordial solar nebula, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Convective accretion disk model for the primordial solar nebula will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-991644