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Relevant bibliographies by topics / PSR J0855-4644

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Academic literature on the topic 'PSR J0855-4644'

Author: Grafiati

Published: 4 June 2021

Last updated: 2 February 2022

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Journal articles on the topic "PSR J0855-4644"

1

Maitra, C., S. Roy, F. Acero, and Y. Gupta. "Discovery of a radio nebula around PSR J0855−4644." Monthly Notices of the Royal Astronomical Society: Letters 477, no. 1 (2018): L66—L69. http://dx.doi.org/10.1093/mnrasl/sly038.

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Bao, Yiwei, Yang Chen, and Siming Liu. "Is PSR J0855−4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?" Monthly Notices of the Royal Astronomical Society 500, no. 4 (2020): 4573–77. http://dx.doi.org/10.1093/mnras/staa3311.

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ABSTRACT DAMPE observation on the cosmic ray electron spectrum hints a narrow excess at ∼1.4 TeV. Although the excess can be ascribed to dark matter particles, pulsars and pulsar wind nebulae are believed to be more natural astrophysical origins: electrons injected from nearby pulsars at their early ages can form a bump-like feature in the spectrum due to radiative energy losses. In this paper, with a survey of nearby pulsars, we filter out four pulsars that may have notable contributions to ∼1.4 TeV cosmic ray electrons. Among them, PSR J0855−4644 has a spin-down luminosity more than 50 times

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3

Maitra, C., F. Acero, and C. Venter. "Constraining the geometry of PSR J0855−4644: A nearby pulsar wind nebula with double torus/jet morphology." Astronomy & Astrophysics 597 (January 2017): A75. http://dx.doi.org/10.1051/0004-6361/201628998.

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Aims. PSR J0855−4644 is a fast-spinning, energetic pulsar discovered at radio wavelengths near the south-eastern rim of the supernova remnant RX J0852.0−4622. A follow-up XMM-Newton observation revealed the X-ray counterpart of the pulsar and a slightly asymmetric pulsar wind nebula, which suggests possible jet structures. Lying at a distance d ≤ 900 pc, PSR J0855−4644 is a pulsar with one of the highest Ė/d2 from which no GeV γ-ray pulsations have been detected. With a dedicated Chandra observation we aim to further resolve the possible jet structures of the nebula and study the pulsar geomet

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4

Redman, M. P., and J. Meaburn. "A possible association of a young pulsar (PSR J0855−4644) with the young Vela supernova remnant RX J0852.0−4622." Monthly Notices of the Royal Astronomical Society 356, no. 3 (2005): 969–73. http://dx.doi.org/10.1111/j.1365-2966.2004.08523.x.

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5

Abdalla, H., A. Abramowski, F. Aharonian, et al. "Deeper H.E.S.S. observations of Vela Junior (RX J0852.0−4622): Morphology studies and resolved spectroscopy." Astronomy & Astrophysics 612 (April 2018): A7. http://dx.doi.org/10.1051/0004-6361/201630002.

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Aims. We study γ-ray emission from the shell-type supernova remnant (SNR) RX J0852.0−4622 to better characterize its spectral properties and its distribution over the SNR.Methods. The analysis of an extended High Energy Spectroscopic System (H.E.S.S.) data set at very high energies (E > 100 GeV) permits detailed studies, as well as spatially resolved spectroscopy, of the morphology and spectrum of the whole RX J0852.0−4622 region. The H.E.S.S. data are combined with archival data from other wavebands and interpreted in the framework of leptonic and hadronic models. The joint Fermi-LAT-H.E.S

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Dissertations / Theses on the topic "PSR J0855-4644"

1

Paz, Arribas Manuel. "Estimation of trigger rates, data rates and data volumes for CTA and observations of SNR RX J0852.0−4622 with H.E.S.S." Doctoral thesis, Humboldt-Universität zu Berlin, 2017. http://dx.doi.org/10.18452/18056.

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Die vorliegende Arbeit beschäftigt sich mit zwei Aspekten der Gammastrahlungsastronomie. Einerseits studiert sie die Anforderungen an das zukünftige CTA-Observatorium für Gammastrahlung und präsentiert insbesondere Abschätzungen der Datenmengen, die während des Betriebs des Observatoriums anfallen werden. Für das größere CTA-Teleskopfeld auf der Südhalbkugel werden demnach eine Triggerate von 13 kHz und Datenraten von bis zu 2500 MB/s erwartet. Unter der Annahme, dass 15% der Zeit für Beobachtungen genutzt werden können, ergibt sich in 15 Jahren ein Datenvolumen von bis zu 165 PB. Die Implem

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