XIPE: the X-ray imaging polarimetry explorer

Soffitta, P.; Barcons, X.; Bellazzini, R.; Braga, J.; Costa, E.; Fraser, George W.; Gburek, S.; Huovelin, J.; Matt, Giorgio; Pearce, Mark; Poutanen, Juri; Reglero, V.; Santangelo, A.; Sunyaev, R.; Tagliaferri, G.; Weisskopf, Martin C.; Aloisio, Roberto; Amato, Elena; Attinà, Primo; Axelsson, M.; Baldini, Luca; Basso, S.; Bianchi, S.; Blasi, Pasquale; Bregeon, J.; Brez, A.; Bucciantini, N.; Burderi, L.; Burwitz, V.; Casella, P.; Churazov, E.; Civitani, M.; Covino, S.; Silva, R. M. Curado da; Cusumano, G.; Dadina, M.; D'Amico, F.; Rosa, A. De; Cosimo, Sergio Di; Persio, Giuseppe Di; Salvo, T. Di; Dovčiak, Michal; Elsner, Ronald F.; Eyles, C. J.; Fabian, A. C.; Fabiani, Sergio; Feng, Hua; Giarrusso, S.; Goosmann, R. W.; Grandi, P.; Grosso, N.; Israel, G. L.; Jackson, M. S.; Kaaret, Philip; Karas, V.; Kuss, M.; Lai, Dong; Rosa, G. La; Larsson, Josefin; Larsson, Stefan; Latronico, L.; Maggio, A.; Maia, J.M.; Marin, Frédéric; Massai, M.M.; Mineo, T.; Minuti, M.; Moretti, E.; Muleri, Fabio; O’Dell, Stephen L.; Pareschi, G.; Peres, G.; Pesce, Melissa; Petrucci, Pierre-Olivier; Pinchera, Michele; Porquet, D.; Ramsey, Brian D.; Rea, N.; Reale, F.; Rodrigo, J. M.; Różáńska, A.; Rubini, A.; Rudawy, P.; Ryde, F.; Salvati, M.; Júnior, Valdivino Alexandre de Santiago; Sazonov, S.; Sgrò, C.; Silver, E.; Spandre, G.; Spiga, D.; Stella, L.; Tamagawa, Toru; Tamborra, F.; Tavecchio, F.; Dias, T.H.V.T.; Adelsberg, Matthew van; Wu, Kinwah; Zane, S.

doi:10.1007/s10686-013-9344-3

Cited by 117 publications

(55 citation statements)

References 173 publications

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“…The major problem with optical emission is that there is usually a large foreground, often polarized (see for example the polarization analysis of the Crab nebula presented in Hester 2008), and the jet-torus structure, which is so prominent in X-ray, is much fainter. Ideally one would like to probe these systems using X-ray polarimetry (Bucciantini 2010), and there is a large interest in the scientific community for such objective (Soffitta et al 2013;Weisskopf et al 2016). Incidentally, the Crab nebula is at the moment the only object with a polarization detected in X-ray (Weisskopf et al 1978).…”

Section: Introductionmentioning

confidence: 99%

Modeling the effect of small-scale magnetic turbulence on the X-ray properties of Pulsar Wind Nebulae

Bucciantini

Bandiera

Olmi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Pulsar Wind Nebulae (PWNe) constitute an ideal astrophysical environment to test our current understanding of relativistic plasma processes. It is well known that magnetic fields play a crucial role in their dynamics and emission properties. At present, one of the main issues concerns the level of magnetic turbulence present in these systems, which in the absence of space resolved X-ray polarization measures cannot be directly constrained. In this work we investigate, for the first time using simulated synchrotron maps, the effect of a small scale fluctuating component of the magnetic field on the emission properties in X-ray. We illustrate how to include the effects of a turbulent component in standard emission models for PWNe, and which consequences are expected in terms of net emissivity and depolarization, showing that the X-ray surface brightness maps can provide already some rough constraints. We then apply our analysis to the Crab and Vela nebulae and, by comparing our model with Chandra and Vela data, we found that the typical energies in the turbulent component of the magnetic field are about 1.5 to 3 times the one in the ordered field.

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Section: Introductionmentioning

confidence: 99%

Modeling the effect of small-scale magnetic turbulence on the X-ray properties of Pulsar Wind Nebulae

Bucciantini

Bandiera

Olmi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…As the perturbative QED is not valid for such field values, it gives overestimated result for delay. This feature can be noted in planning of future astrophysical missions aimed at the QED effects investigation in the pulsar fields, such as XIPE [28].…”

Section: Jhep05(2017)105mentioning

confidence: 89%

Nonperturbative QED vacuum birefringence

Денисов

Dolgaya

Соколов

2017

J. High Energ. Phys.

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In this paper we represent nonperturbative calculation for one-loop Quantum Electrodynamics (QED) vacuum birefringence in presence of strong magnetic field. The dispersion relations for electromagnetic wave propagating in strong magnetic field point to retention of vacuum birefringence even in case when the field strength greatly exceeds Sauter-Schwinger limit. This gives a possibility to extend some predictions of perturbative QED such as electromagnetic waves delay in pulsars neighbourhood or wave polarization state changing (tested in PVLAS) to arbitrary magnetic field values. Such expansion is especially important in astrophysics because magnetic fields of some pulsars and magnetars greatly exceed quantum magnetic field limit, so the estimates of perturbative QED effects in this case require clarification.

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“…Coupled to a low X-ray luminosity, such degree of polarization is, by any standard, by far too low to be detected with the current generation of X-ray polarimeters. Such statement includes the Gas Pixel Detector technology (Soffitta et al 2013), Time Projection Chamber polarimeter concepts (Black et al 2010), and polarimeters based on Bragg diffraction and Thomson scattering (Kaaret et al 1989). Note that most of those polarimeter concepts are also limited to energies higher than 0.7 keV.…”

Section: Is Direct Detection Of the Exoplanet In X-rays Possible?mentioning

confidence: 99%

Computation of the Transmitted and Polarized Scattered Fluxes by the Exoplanet HD 189733b in X-Rays

Marin

Grosso

2017

ApJ

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Thousands of exoplanets have been detected, but only one exoplanetary transit was potentially observed in X-rays from HD 189733A. What makes the detection of exoplanets so difficult in this band? To answer this question, we run Monte-Carlo radiative transfer simulations to estimate the amount of X-ray flux reprocessed by HD 189733b Despite its extended evaporating-atmosphere, we find that the X-ray absorption radius of HD 189733b at 0.7 keV, the mean energy of the photons detected in the 0.25-2 keV energy band by XMM-Newton, is ∼1.01 times the planetary radius for an atmosphere of atomic Hydrogen and Helium (including ions), and produces a maximum depth of ∼2.1% at ∼±46 min from the center of the planetary transit on the geometrically thick and optically thin corona. We compute numerically in the 0.25-2 keV energy band that this maximum depth is only of ∼1.6% at ∼±47 min from the transit center, and little sensitive to the metal abundance assuming that adding metals in the atmosphere would not dramatically change the density-temperature profile. Regarding a direct detection of HD 189733b in X-rays, we find that the amount of flux reprocessed by the exoplanetary atmosphere varies with the orbital phase, spanning between 3-5 orders of magnitude fainter than the flux of the primary star. Additionally, the degree of linear polarization emerging from HD 189733b is <0.003%, with maximums detected near planetary greatest elongations. This implies that both the modulation of the X-ray flux with the orbital phase and the scattered-induced continuum polarization cannot be observed with current X-ray facilities.

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XIPE: the X-ray imaging polarimetry explorer

Cited by 117 publications

References 173 publications

Modeling the effect of small-scale magnetic turbulence on the X-ray properties of Pulsar Wind Nebulae

Modeling the effect of small-scale magnetic turbulence on the X-ray properties of Pulsar Wind Nebulae

Nonperturbative QED vacuum birefringence

Computation of the Transmitted and Polarized Scattered Fluxes by the Exoplanet HD 189733b in X-Rays

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