Magnetar Twists: Fermi / GBM Detec5on of SGR 1550‐5418 Ersin Göğüş Sabancı University, Istanbul Yuki Kaneko C. Kouveliotou, E. Ramirez‐Ruiz, J. Granot, A. van der Horst, A. WaYs, A. von Kienlin, et al. Fermi Symposium, Washington, D.C. November 4, 2009
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Magnetar Twists: Fermi / GBM Detecon of SGR 1550‐5418 · Magnetar Twists: Fermi / GBM Detecon of SGR 1550‐5418 Ersin Göğüş Sabancı University, Istanbul Yuki Kaneko C. Kouveliotou,
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e± plasmas & photons confined by closed B field region
Trapped energy: EB(a) = 1/6 a3B2 > Eiso,BB
For a = 120 m & Eiso,BB= 5.6 × 1040 erg: B > 1.4 × 1014 G
consistent with B = 2.2 x 1014 G from PP
Energy dissipated in the corona is radiated in two forms:
non-thermal, high energy radiation produced by collisionless dissipation of the coronal beam
blackbody radiation by thermalization: as the remaining energy dissipated in the corona enters the dense atmosphere, the crust is thermalized by two-body collisions and e-/e+ pair formation
Both components are expected to have comparable luminosities.