Black-Hole Transients and the Eddington Limit
classification
🌌 astro-ph
keywords
black-holecriticaleddingtonlimitperiodappearbehaviourbeyond
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I show that the Eddington limit implies a critical orbital period P_crit(BH) = 2d beyond which black-hole LMXBs cannot appear as persistent systems. The unusual behaviour of GRO J1655-40 may result from its location close to this critical period.
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