Multi-Wavelength Polarimetry of Isolated Pulsars

Hard X-ray Polarimetry -- An overview of the method, science drivers and recent findings

“…BH spin, inclination, study of accretion disk dynamics, GR effects from polarized thermal disk emission (Dovčiak et al, 2008;Schnittman & Krolik, 2009) ∼1-3 % A few % of PF for Cygnus X-1 in high soft state (Long et al, 1980) IXPE (2021) (Weisskopf et al, 2016;Soffitta, 2017), EXTP (Zhang et al, 2016), SOLPEX (Ste ¸ślicki et al, 2016) Blazars First peak of HBL (faint in this energy range) − Jet structure, magnetic field geometry (Zhang et al, 2014;Tavecchio et al, 2018) a few to high % depending on the B field geometry Magnetars Vacuum birefringence, signature of RICS (Taverna et al, 2014) ∼20 % XRP Emission mechanism, geometry -Polar cap/Outer gap/slot gap/striped wind models (Weisskopf et al, 2009;Harding, 2019) a few tens of % ∼15 % PF for Crab+nebula by PolarLight (Feng et al, 2020) SNR, PWN Particle acceleration process in shocks, magnetic field geometry (Bykov et al, 2009) ∼20-50 % from different regions of SNR ∼19 % PF for Crab nebula by OSO-8 (Weisskopf et al, 1978). ∼14 % PF by PolarLight (Feng et al, 2020) 10−100 keV…”

“…Corona and torus geometry (Schnittman & Krolik, 2010;Goosmann & Matt, 2011) ∼10 % Blazars Second peak of LBL: SSC/ EC/hadronic models (McNamara et al, 2009;Zhang & Böttcher, 2013) a few % (EC) to 50 % (SSC) XRP Emission mechanism, geometry -Polar cap/Outer gap/slot gap/striped wind models (Weisskopf et al, 2009;Harding, 2019) A few tens of % ∼21 % PF for Crab+nebula by PoGO+ (Chauvin et al, 2018b), ∼22 % PF by Hitomi (Aharonian et al, 2018) Magnetars Signature of RICS from polarized hard X-ray tail (Wadiasingh et al, 2019) APP 3 Beam shape (pencil/fan beam models) from phase resolved polarimetry near cyclotron energies. Magnetic field, accretion column geometry from accretion shock/disk scattered emission (Meszaros et al, 1988) up to 30 % PWN Acceleration mechanism and magnetic field geometry (Weisskopf et al, 2009;Harding, 2019) ∼20-30 % ∼17.4 % PF for Crab nebula by PoGO+ (Chauvin et al, 2018b) Solar flares Emission mechanism, electron beaming, magnetic field structure for M and X class flares (Bai & Ramaty, 1978;Leach et al, 1985;Zharkova et al, 2010) ∼35-50 % for flares away from Sun's center ∼8-40 % PF for 25 flares by CORONAS-F (Zhitnik et al, 2006) 100−1000 keV…”