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http://hdl.handle.net/2445/175202
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DC Field | Value | Language |
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dc.contributor.author | Bosch i Ramon, Valentí | - |
dc.date.accessioned | 2021-03-17T09:26:32Z | - |
dc.date.available | 2021-03-17T09:26:32Z | - |
dc.date.issued | 2021-01-13 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.uri | http://hdl.handle.net/2445/175202 | - |
dc.description.abstract | Context. LS 5039 is a powerful high-mass gamma-ray binary that probably hosts a young non-accreting pulsar. However, despite the wealth of data available, the means by which the non-thermal emitter is powered are still unknown. Aims. We use a dynamical-radiative numerical model, and multiwavelength data, to constrain the properties of a hypothetical pulsar wind that would power the non-thermal emitter in LS 5039. Methods. We ran simulations of an ultrarelativistic (weakly magnetized) cold e±-wind that Compton scatters stellar photons and that dynamically interacts with the stellar wind. The effects of energy losses on the unshocked e±-wind dynamics, and the geometry of the two-wind contact discontinuity, are computed for different wind models. The predicted unshocked e±-wind radiation at periastron, when expected to be the highest, is compared to LS 5039 data. Results. The minimum possible radiation from an isotropic cold e±-wind overpredicts the X-ray to gamma-ray fluxes at periastron by a factor of ∼3. In the anisotropic (axisymmetric) wind case X-ray and ≳100 MeV data are not violated by wind radiation if the wind axis is at ≲20−40° from the line of sight (chance probability of ≲6−24%), depending on the anisotropic wind model, or if the wind Lorentz factor ∈102 − 103, in which case the wind power can be higher, but it requires e±-multiplicities of ∼106 and 109 for a 10−2 s and 10 s pulsar period, respectively. Conclusions. The studied model predicts that a weakly magnetized cold pulsar e±-wind in LS 5039 should be strongly anisotropic, with either a wind Lorentz factor ∈102 − 103 and very high multiplicities or with a fine-tuned wind orientation. A weakly magnetized, cold baryon-dominated wind would be a possible alternative, but then the multiplicities should be rather low, while the baryon-to-e± energy transfer should be very efficient at wind termination. A strongly magnetized cold wind seems to be the most favorable option as it is consistent with recent research on pulsar winds and does not require fine-tuning of the pulsar wind orientation, and the wind multiplicity and Lorentz factor are less constrained. | - |
dc.format.mimetype | application/pdf | - |
dc.language.iso | eng | - |
dc.publisher | EDP Sciences | - |
dc.relation.isformatof | Reproducció del document publicat a: https://doi.org/10.1051/0004-6361/202039666 | - |
dc.relation.ispartof | Astronomy & Astrophysics, 2021, vol. 645, p. 86 | - |
dc.relation.uri | https://doi.org/10.1051/0004-6361/202039666 | - |
dc.rights | (c) The European Southern Observatory (ESO), 2021 | - |
dc.source | Articles publicats en revistes (Física Quàntica i Astrofísica) | - |
dc.subject.classification | Astronomia de raigs gamma | - |
dc.subject.classification | Radiació | - |
dc.subject.classification | Estels | - |
dc.subject.other | Gamma ray astronomy | - |
dc.subject.other | Radiation | - |
dc.subject.other | Stars | - |
dc.title | Properties of a hypothetical cold pulsar wind in LS 5039 | - |
dc.type | info:eu-repo/semantics/article | - |
dc.type | info:eu-repo/semantics/publishedVersion | - |
dc.identifier.idgrec | 709004 | - |
dc.date.updated | 2021-03-17T09:26:33Z | - |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | - |
Appears in Collections: | Articles publicats en revistes (Física Quàntica i Astrofísica) |
Files in This Item:
File | Description | Size | Format | |
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709004.pdf | 2.17 MB | Adobe PDF | View/Open |
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