THE INFLUENCE OF MAGNETIC FIELDS ON THE THERMODYNAMICS OF PRIMORDIAL STAR FORMATION

Journal Article · Sun Sep 20 00:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/703/1/1096· OSTI ID:21371928

Schleicher, Dominik R. G.; Glover, Simon C. O.; Banerjee, Robi; Klessen, Ralf S ^[1]; Galli, Daniele; Palla, Francesco; Schneider, Raffaella ^[2]

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1. Zentrum fuer Astronomie der Universitaet Heidelberg, Institut fuer Theoretische Astrophysik, Albert-Ueberle-Str. 2, D-69120 Heidelberg (Germany)
2. INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze (Italy)

We explore the effects of magnetic energy dissipation on the formation of the first stars. For this purpose, we follow the evolution of primordial chemistry in the presence of magnetic fields in the post-recombination universe until the formation of the first virialized halos. From the point of virialization, we follow the protostellar collapse up to densities of {approx}10{sup 12} cm{sup -3} in a one-zone model. In the intergalactic medium (IGM), comoving field strengths of {approx}>0.1 nG lead to Jeans masses of 10{sup 8} M {sub sun} or more and thus delay gravitational collapse in the first halos until they are sufficiently massive. During protostellar collapse, we find that the temperature minimum at densities of {approx}10{sup 3} cm{sup -3} does not change significantly, such that the characteristic mass scale for fragmentation is not affected. However, we find a significant temperature increase at higher densities for comoving field strengths of {approx}> 0.1 nG. This may delay gravitational collapse, in particular at densities of {approx}10{sup 9} cm{sup -3}, where the proton abundance drops rapidly and the main contribution to the ambipolar diffusion resistivity is due to collisions with Li{sup +}. We further explore how the thermal evolution depends on the scaling relation of magnetic field strength with density. While the effects are already significant for our fiducial model with B propor to rho{sup 0.5-0.57}, the temperature may increase even further for steeper relations and lead to the complete dissociation of H{sub 2} at densities of {approx}10{sup 11} cm{sup -3} for a scaling with B propor to rho{sup 0.6}. The correct modeling of this relation is therefore very important, as the increase in temperature enhances the subsequent accretion rate onto the protostar. Our model confirms that initial weak magnetic fields may be amplified considerably during gravitational collapse and become dynamically relevant. For instance, a comoving field strength above 10{sup -5} nG will be amplified above the critical value for the onset of jets which can magnetize the IGM.

• OSTI ID: 21371928
• Journal Information: Astrophysical Journal, Vol. 703, Issue 1; Other Information: DOI: 10.1088/0004-637X/703/1/1096; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ABUNDANCE
AMBIPOLAR DIFFUSION
COSMOLOGY
ENERGY LOSSES
GRAVITATIONAL COLLAPSE
HYDROGEN
LITHIUM IONS
MAGNETIC FIELDS
PROTONS
RECOMBINATION
SIMULATION
STARS
THERMODYNAMICS
UNIVERSE
BARYONS
CHARGED PARTICLES
DIFFUSION
ELEMENTARY PARTICLES
ELEMENTS
FERMIONS
HADRONS
IONS
LOSSES
NONMETALS
NUCLEONS