arXiv: High Energy Astrophysical Phenomena最新文献_第6页

Pairs of giant shock waves (N-waves) in merging galaxy clusters 合并星系团中的一对巨大的激波(n波)

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-28 DOI: 10.1093/mnras/staa3718

Congyao Zhang, E. Churazov, I. Zhuravleva

{"title":"Pairs of giant shock waves (N-waves) in merging galaxy clusters","authors":"Congyao Zhang, E. Churazov, I. Zhuravleva","doi":"10.1093/mnras/staa3718","DOIUrl":"https://doi.org/10.1093/mnras/staa3718","url":null,"abstract":"When a subcluster merges with a larger galaxy cluster, a bow shock is driven ahead of the subcluster. At a later merger stage, this bow shock separates from the subcluster, becoming a \"runaway\" shock that propagates down the steep density gradient through the cluster outskirts and approximately maintains its strength and the Mach number. Such shocks are plausible candidates for producing radio relics in the periphery of clusters. We argue that, during the same merger stage, a secondary shock is formed much closer to the main cluster center. A close analog of this structure is known in the usual hydrodynamics as N-waves, where the trailing part of the \"N\" is the result of the non-linear evolution of a shock. In merging clusters, spherical geometry and stratification could further promote its development. Both the primary and the secondary shocks are the natural outcome of a single merger event and often both components of the pair should be present. However, in the radio band, the leading shock could be more prominent, while the trailing shock might conversely be more easily seen in X-rays. The latter argument implies that for some of the (trailing) shocks found in X-ray data, it might be difficult to identify their \"partner\" leading shocks or the merging subclusters, which are farther away from the cluster center. We argue that the Coma cluster and A2744 could be two examples in a post-merger state with such well-separated shock pairs.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"274 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76574642","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 6

Ambipolar decay of magnetic field in magnetars and the observed magnetar activities 磁星磁场的双极衰减与观测到的磁星活动

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-21 DOI: 10.1142/S0217732321501443

B. Bhalla, M. Sinha

引用次数: 1

Unveiling the origin of steep decay in γ-ray bursts 揭示γ射线暴中急剧衰减的起源

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-18 DOI: 10.21203/rs.3.rs-74350/v1

S. Ronchini, G. Oganesyan, M. Branchesi, S. Ascenzi, M. Bernardini, F. Brighenti, S. Dall’Osso, P. D’Avanzo, G. Ghirlanda, G. Ghisellini, M. Ravasio, O. Salafia

{"title":"Unveiling the origin of steep decay in γ-ray bursts","authors":"S. Ronchini, G. Oganesyan, M. Branchesi, S. Ascenzi, M. Bernardini, F. Brighenti, S. Dall’Osso, P. D’Avanzo, G. Ghirlanda, G. Ghisellini, M. Ravasio, O. Salafia","doi":"10.21203/rs.3.rs-74350/v1","DOIUrl":"https://doi.org/10.21203/rs.3.rs-74350/v1","url":null,"abstract":"\u0000 γ-ray bursts (GRBs) are short-lived transients releasing a large amount of energy (10^51-10^53 erg) in the keV-MeV energy range. GRBs are thought to originate from internal dissipation of the energy carried by ultra-relativistic jets launched by the remnant of a massive star’s death or a compact binary coalescence. While thousands of GRBs have been observed over the last thirty years, we still have an incomplete understanding of where and how the radiation is generated in the jet. A novel investigation of the GRB emission mechanism, via time-resolved spectral analysis of the X-ray tails of bright GRB pulses, enables us to discover a unique relation between the spectral index and the flux. This relation is incompatible with the long standing scenario invoked to interpret X-ray tails, that is, the delayed arrival of pho-tons from high-latitude parts of the jet. We show that our results provide for the first time evidence of adiabatic cooling and efficient energy exchange between the emitting particles in the relativistic outflows of GRBs.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89726150","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 1

Type Ia supernovae from wide white dwarfs triples Ia型超新星来自三倍宽的白矮星

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-16 DOI: 10.1093/mnras/staa3623

E. Michaely

引用次数: 5

Exploring the effects of magnetar bursts in pulsar wind nebulae 探索脉冲星风星云中磁星爆发的影响

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-16 DOI: 10.1016/j.jheap.2020.09.001

J. Martin, D. Torres, Bing Zhang

引用次数: 2

Neutron conversion–diffusion: a new model for structured short gamma-ray burst jets compatible with GRB 170817 中子转换-扩散:与GRB 170817兼容的结构短伽马暴射流新模型

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-16 DOI: 10.1093/MNRAS/STAB652

Edwan Pr'eau, K. Ioka, P. M'esz'aros

引用次数: 1

Formation of binary black holes similar to GW190521 with a total mass of ∼150 M⊙ from Population III binary star evolution 类似于GW190521的双黑洞，总质量约150 M⊙，来自星族III双星演化

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-15 DOI: 10.1093/mnrasl/slaa191

T. Kinugawa, Takashi Nakamura, H. Nakano

引用次数: 41

Choked accretion onto a Kerr black hole 克尔黑洞的窒息吸积

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-14 DOI: 10.1103/physrevd.103.023003

A. Aguayo-Ortiz, O. Sarbach, E. Tejeda

引用次数: 4

A Relativistic Orbit Model for Temporal Properties of AGN AGN时间性质的相对论轨道模型

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-09-07 DOI: 10.3390/galaxies8030067

P. Rana, A. Mangalam

{"title":"A Relativistic Orbit Model for Temporal Properties of AGN","authors":"P. Rana, A. Mangalam","doi":"10.3390/galaxies8030067","DOIUrl":"https://doi.org/10.3390/galaxies8030067","url":null,"abstract":"We present a unified model for X-ray quasi-periodic oscillations (QPOs) seen in Narrow-line Seyfert 1 (NLSy1) galaxies, $gamma$-ray and optical band QPOs that are seen in Blazars. The origin of these QPOs is attributed to the plasma motion in corona or jets of these AGN. In the case of X-ray QPOs, we applied the general relativistic precession model for the two simultaneous QPOs seen in NLSy1 1H 0707-945 and deduce orbital parameters, such the radius of the emission region, and spin parameter $a$ for a circular orbit; we obtained the Carter's constant $Q$, $a$, and the radius in the case of a spherical orbit solution. In other cases where only one X-ray QPO is seen, we localized the orbital parameters for NLSy1 galaxies REJ 1034+396, 2XMM J123103.2+110648, MS 2254.9-3712, Mrk 766, and MCG-06-30-15. By applying the lighthouse model, we found that a kinematic origin of the jet based $gamma$-ray and optical QPOs, in a relativistic MHD framework, is possible. Based on the inbuilt Hamiltonian formulation with a power-law distribution in the orbital energy of the plasma consisting of only circular or spherical trajectories, we show that the resulting Fourier power spectral density (PSD) has a break corresponding to the energy at ISCO. Further, we derive connection formulae between the slopes in the PSD and that of the energy distribution. Overall, given the preliminary but promising results of these relativistic orbit models to match the observed QPO frequencies and PSD at diverse scales in the inner corona and the jet, it motivates us to build detailed models, including a transfer function for the energy spectrum in the corona and relativistic MHD jet models for plasma flow and its polarization properties.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"68 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77896011","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 2

Muonization of supernova matter 超新星物质的介子化

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-08-31 DOI: 10.1103/physrevd.102.123001

T. Fischer, G. Guo, G. Mart'inez-Pinedo, M. Liebendörfer, A. Mezzacappa

引用次数: 17