Large Convective Events And Their Aftermath In A Rotating Star

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A global model of the magnetorotational instability in

the large rotational energy of a protoneutron star (PNS) rotating with a period of a few milliseconds. The presence of a magnetic field can impact the explosion by converting the energy of di er-ential rotation into thermal energy (Thompson et al. 2005) and/or into a large-scale magnetic field, which can launch jets and lead

The Spin Evolution of Fast-rotating, Magnetized Super

The Spin Evolution of Fast-rotating, Magnetized Super-Chandrasekhar White Dwarfs in the Aftermath of White Dwarf Mergers L. Becerra1,2, J. A. Rueda1,2,3, P. Lorén-Aguilar4, and E. García-Berro5,6 1 Dipartimento di Fisica, Sapienza Università di Roma, P.le Aldo Moro 5, I-00185 Rome, Italy 2 ICRANet, P.zza della Repubblica 10, I-65122 Pescara

A global model of the magnetorotational instability in

Context. Magnetars are isolated neutron stars characterized by their variable high-energy emission, which is powered by the dissipa-tion of enormous internal magnetic fields. The measured spin-down of magnetars constrains the magnetic dipole to be in the range of 10141015 G. The magnetorotational instability (MRI) is considered to be a

An unusual white dwarf star may be a surviving remnant of a

365. However, only ∼ 10−8 such events are expected per year in the Milky Way (31) compared to a rate of ∼ 10−3 for SN Iax events (32); therefore this scenario is less probable. The actual donor star that mustalso have been ejected (21) along with LP 40-365 should be detectable as well.

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Still, applying the techniques that have proved so successful in the study of red giants to their higher-mass cousins could still shed new light on the behavior of their outer layers. Trying to quantify the distinct contributions from convective variations, mass loss events, changes in circumstellar dust content, pulsations, and other crucial