Computer Science – Numerical Analysis
Scientific paper
Oct 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasj...45..715k&link_type=abstract
PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 45, no. 5, p. 715-725
Computer Science
Numerical Analysis
24
Accretion Disks, F Stars, Numerical Analysis, Stability, T Tauri Stars, Data Reduction, Light Curve, Stellar Mass Ejection, Stellar Structure, Stellar Temperature, Thermal Stability
Scientific paper
According to the theory of the thermal limit-cycle instability in the partial ionization zone of hydrogen in accretion disks, the inner portions of the disks in FU Ori stars are unstable. We have demonstrated by means of one-dimensional numerical simulations that for a steady mass input of dot-Minput approximately 10-5 solar mass/yr, the instability develops in the inner portions of the disk (at less than 1 AU), thereby modulating the mass-accretion rate onto a central star between dot-Macc = 10-4 solar mass/yr, a typical accretion rate in FU Ori stars, and dot-Macc less than or approximately = 10-7 solar mass/yr, a characteristic rate of the usual T Tauri stars. The outburst recurrence times are roughly trec approximately 4000 (yr) (alpha/10-4)-0.8 with alpha being the viscosity parameter. The duty cycle, the fraction of the outburst duration to the period of one limit cycle, is approximately 0.1. The disks in the T Tau phase are far from being in a steady state, and relatively flat spectra (nu fnu approximately constant) are formed at near infrared-optical wavelengths. When the mass input rate drops below 10-7 solar mass/yr in the pre-main-sequence stellar evolution, since entire portions of the disk become thermally stable, the limit-cycle behavior ceases to appear.
Kawazoe Eiko
Mineshige Shin
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