arXiv: High Energy Astrophysical Phenomena最新文献_第3页

Fresnel models for gravitational wave effects on pulsar timing 引力波对脉冲星计时影响的菲涅耳模型

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-18 DOI: 10.1093/mnras/stab1417

C. McGrath, J. Creighton

引用次数: 2

Colliding stellar wind modelling of the X-ray emission from WR 140 WR 140 x射线辐射的碰撞恒星风模型

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-17 DOI: 10.1093/mnras/staa3591

S. Zhekov

引用次数: 3

Modeling and searching for a stochastic gravitational-wave background from ultralight vector bosons 超轻矢量玻色子的随机引力波背景建模与搜索

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-13 DOI: 10.1103/PhysRevD.103.083005

Leo Tsukada, R. Brito, W. East, Nils Siemonsen

{"title":"Modeling and searching for a stochastic gravitational-wave background from ultralight vector bosons","authors":"Leo Tsukada, R. Brito, W. East, Nils Siemonsen","doi":"10.1103/PhysRevD.103.083005","DOIUrl":"https://doi.org/10.1103/PhysRevD.103.083005","url":null,"abstract":"Ultralight bosons, which are predicted in a variety of beyond-Standard-Model scenarios as dark-matter candidates, can trigger the superradiant instability around spinning black holes. This instability gives rise to oscillating boson condensates which then dissipate through the emission of nearly monochromatic gravitational waves. Such systems are promising sources for current and future gravitational-wave detectors. In this work, we consider minimally-coupled, massive vector bosons, which can produce a significantly stronger gravitational-wave signal compared to the scalar case. We adopt recently obtained numerical results for the gravitational-wave flux, and astrophysical models of black hole populations that include both isolated black holes and binary merger remnants, to compute and study in detail the stochastic gravitational-wave background emitted by these sources. Using a Bayesian framework, we search for such a background signal emitted using data from the first and second observing runs of Advanced LIGO. We find no evidence for such a signal. Therefore, the results allow us to constrain minimally coupled vector fields with masses in the range $0.8times10^{-13}mathrm{eV}leq m_bleq 6.0times10^{-13}mathrm{eV}$ at 95% credibility, assuming optimistically that the dimensionless spin distribution for the isolated black hole population is uniform in the range $[0,1]$. With more pessimistic assumptions, a narrower range around $m_bapprox 10^{-13}mathrm{eV}$ can still be excluded as long as the upper end of the uniform distribution for dimensionless black hole spin is $gtrsim 0.2$.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76855857","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: 23

The non-relativistic interiors of ultra-relativistic explosions: Extension to the Blandford–McKee solutions 超相对论性爆炸的非相对论性内部:对Blandford-McKee解的扩展

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-11 DOI: 10.1063/5.0037299

T. Faran, R. Sari

引用次数: 2

New measurements of the cyclotron line energy in Cen X-3 半人马座X-3回旋加速器线能量的新测量

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-11 DOI: 10.1093/mnras/staa3477

Gunjan Tomar, P. Pradhan, B. Paul

{"title":"New measurements of the cyclotron line energy in Cen X-3","authors":"Gunjan Tomar, P. Pradhan, B. Paul","doi":"10.1093/mnras/staa3477","DOIUrl":"https://doi.org/10.1093/mnras/staa3477","url":null,"abstract":"We report results from the analysis of data from two observations of the accreting binary X-ray pulsar Cen X-3 carried out with the broadband X-ray observatories Suzaku and NuSTAR. The pulse profile is dominated by a broad single peak and show some energy dependence with two additional weak pulse peaks at energies below 15 and 25 keV respectively. The broadband X-ray spectrum for 0.8-60.0 keV for Suzaku and 3.0-60.0 keV for NuSTAR is fitted well with high energy cut-off power-law model along with soft-excess, multiple iron emission lines and a cyclotron absorption. The cyclotron line energy is found to be $30.29^{+0.68}_{-0.61}$ keV and $29.22^{+0.28}_{-0.27}$ keV respectively in the Suzaku and NuSTAR spectra. We make a comparison of these two measurements with four previous measurements of CRSF in Cen X-3 obtained with Ginga, BeppoSAX and RXTE. We find no evidence for a dependence of the CRSF on luminosity. Except for one CRSF measurement with BeppoSAX, the remaining measurements are consistent with a CRSF energy in the range of 29.5 - 30.0 keV over a luminosity range of 1.1-5.4 $times 10^{37}$ ergs s$^{-1}$ different from several other sources that show considerable CRSF variation in the same luminosity range.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"40 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80954858","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: 4

Follow-up observations for IceCube-170922A: Detection of rapid near-infrared variability and intensive monitoring of TXS 0506+056 IceCube-170922A的后续观测:探测TXS 0506+056的快速近红外变型和强化监测

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-10 DOI: 10.1093/PASJ/PSAA110

T. Morokuma, Y. Utsumi, K. Ohta, M. Yamanaka, K. Kawabata, Y. Inoue, Masaomi Tanaka, Michitoshi Yoshida, R. Itoh, M. Sasada, N. Tominaga, Hiroki Mori, M. Kawabata, T. Nakaoka, Maiko Chogi, T. Abe, Ruochen Huang, N. Kawahara, Hiroki Kimura, H. Nagashima, K. Takagi, Y. Yamazaki, Wei Liu, R. Ohsawa, S. Sako, K. Murata, K. Morihana, C. Gilligan, K. Isogai, M. Kimura, Yasuyuki Wakamatsu, Ryuhei Ohnishi, M. Takayama, S. Honda, Y. Matsuoka, T. Yamashita, S. Nagataki, Yasuyuki T. Tanaka

{"title":"Follow-up observations for IceCube-170922A: Detection of rapid near-infrared variability and intensive monitoring of TXS 0506+056","authors":"T. Morokuma, Y. Utsumi, K. Ohta, M. Yamanaka, K. Kawabata, Y. Inoue, Masaomi Tanaka, Michitoshi Yoshida, R. Itoh, M. Sasada, N. Tominaga, Hiroki Mori, M. Kawabata, T. Nakaoka, Maiko Chogi, T. Abe, Ruochen Huang, N. Kawahara, Hiroki Kimura, H. Nagashima, K. Takagi, Y. Yamazaki, Wei Liu, R. Ohsawa, S. Sako, K. Murata, K. Morihana, C. Gilligan, K. Isogai, M. Kimura, Yasuyuki Wakamatsu, Ryuhei Ohnishi, M. Takayama, S. Honda, Y. Matsuoka, T. Yamashita, S. Nagataki, Yasuyuki T. Tanaka","doi":"10.1093/PASJ/PSAA110","DOIUrl":"https://doi.org/10.1093/PASJ/PSAA110","url":null,"abstract":"We present our follow-up observations to search for an electromagnetic counterpart of the IceCube high-energy neutrino, IceCube-170922A. Monitoring observations of a likely counterpart, TXS 0506+056, are also described. First, we quickly took optical and near-infrared images of 7 flat-spectrum radio sources within the IceCube error region right after the neutrino detection and found a rapid flux decline of TXS 0506+056 in Kanata/HONIR J-band data. Motivated by this discovery, intensive follow-up observations of TXS 0506+056 are continuously done, including our monitoring imaging observations, spectroscopic observations, and polarimetric observations in optical and near-infrared wavelengths. TXS 0506+056 shows a large amplitude (~1.0 mag) variability in a time scale of several days or longer, although no significant variability is detected in a time scale of a day or shorter. TXS 0506+056 also shows a bluer-when-brighter trend in optical and near-infrared wavelengths. Structure functions of variabilities are examined and indicate that TXS 0506+056 is not a special blazar in terms of optical variability. Polarization measurement results of TXS 0506+056 are also discussed.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88570502","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

Constraining the shear acceleration model for the X-ray emission of large-scale extragalactic jets 约束大尺度河外喷流x射线发射的剪切加速度模型

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-06 DOI: 10.1093/mnras/staa4009

F. Tavecchio

{"title":"Constraining the shear acceleration model for the X-ray emission of large-scale extragalactic jets","authors":"F. Tavecchio","doi":"10.1093/mnras/staa4009","DOIUrl":"https://doi.org/10.1093/mnras/staa4009","url":null,"abstract":"The nature of the intense X-ray emission from powerful extragalactic jets at large ($>1$ kpc) scale is still debated. The scenario that invokes the inverse Compton scattering of the CMB by electrons is challenged by the lack of gamma-ray emission in the GeV band. An alternative assumes synchrotron emission by a distinct population of ultra-high energy electrons. Here we present a concrete attempt to apply this scenario, exploring the specific model in which the ultra-high energy electrons are accelerated in a shear layer surrounding the jet. We limit the study to non-relativistic flows and particle acceleration is treated by a Fokker-Planck equation. The strict spatial coincidence between low energy (radio, optical) and X-ray emission prompts us to assume that the required population of pre-accelerated particles is provided by a shock responsible for the acceleration of the electrons emitting at low frequencies. We apply the model to the emission of the principal knots of the jets of PKS 0637-752 and PKS 1136-135, two of the best studied objects. For the set of fiducial parameters adopted, the condition that the jet power does not exceeds a limiting value of $10^{48}$ erg s$^{-1}$ constrains the magnetic field above $10$ $mu$G and indicates moderate beaming ($deltasimeq 2$) for PKS 0637-752. For both sources, the requirement that acceleration of the electrons proceeds faster than radiative cooling can be met if the magnetic turbulence in the shear layer follows a Kolmogorov spectrum, $I(k)propto k^{-q}$ with $q=5/3$, but cannot satisfied in the Bohm-like case ($q=1$).","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"50 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74251376","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: 10

Understanding and improving the timing of PSR J0737−3039B 了解并改进PSR J0737−3039B的时序

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-03 DOI: 10.1051/0004-6361/202038566

A. Noutsos, G. Desvignes, M. Kramer, N. Wex, P. Freire, I. Stairs, M. Mclaughlin, R. Manchester, A. Possenti, M. Burgay, A. Lyne, R. Breton, B. Perera, R. Ferdman

{"title":"Understanding and improving the timing of PSR J0737−3039B","authors":"A. Noutsos, G. Desvignes, M. Kramer, N. Wex, P. Freire, I. Stairs, M. Mclaughlin, R. Manchester, A. Possenti, M. Burgay, A. Lyne, R. Breton, B. Perera, R. Ferdman","doi":"10.1051/0004-6361/202038566","DOIUrl":"https://doi.org/10.1051/0004-6361/202038566","url":null,"abstract":"The double pulsar (PSR J0737-3039A/B) provides some of the most stringent tests of general relativity (GR) and its alternatives. The success of this system in tests of GR is largely due to the high-precision, long-term timing of its recycled-pulsar member, pulsar A. On the other hand, pulsar B is a young pulsar that exhibits significant short-term and long-term timing variations due to the electromagnetic-wind interaction with its companion and geodetic precession. Improving pulsar B's timing precision is a key step towards improving the precision in a number of GR tests with PSR J0737-3039A/B. In this paper, red noise signatures in the timing of pulsar B are investigated using roughly a four-year time span, from 2004 to 2008, beyond which time the pulsar's radio beam precessed out of view ... The timing of pulsar B presented in this paper depends on the size of the pulsar's orbit, which was calculated from GR, in order to precisely account for orbital timing delays. Consequently, our timing cannot directly be used to test theories of gravity. However, our modelling of the beam shape and radial wind of pulsar B can indirectly aid future efforts to time this pulsar by constraining part of the additional red noise observed on top of the orbital delays. As such, we conclude that, in the idealised case of zero covariance between our model's parameters and those of the timing model, our model can bring about a factor 2.6 improvement on the measurement precision of the mass ratio, R = mA/mB, between the two pulsars: a theory-independent parameter, which is pivotal in tests of GR.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"12 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80142781","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: 7

Supermassive neutron stars rule out twin stars 超大质量中子星排除了双星的可能性

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-02 DOI: 10.1103/PhysRevD.103.063042

J. Christian, J. Schaffner-Bielich

引用次数: 12

Spinning black holes as cosmic string factories 旋转黑洞是宇宙弦工厂

arXiv: High Energy Astrophysical Phenomena Pub Date : 2020-11-02 DOI: 10.1103/PHYSREVD.103.083019

Hengrui Xing, Y. Levin, A. Gruzinov, A. Vilenkin

{"title":"Spinning black holes as cosmic string factories","authors":"Hengrui Xing, Y. Levin, A. Gruzinov, A. Vilenkin","doi":"10.1103/PHYSREVD.103.083019","DOIUrl":"https://doi.org/10.1103/PHYSREVD.103.083019","url":null,"abstract":"We consider the evolution of a cosmic string loop that is captured by a much more massive and compact black hole. We show that after several reconnections that produce ejections of smaller loops, the loop that remains bound to the black hole moves on a nearly-periodic non-self-intersecting trajectory, \"the orbit\". The orbit evolves due to an energy and angular momentum exchange between the loop and the spinning black hole. We show that such evolution is mathematically equivalent to a certain continuous deformation of an auxiliary closed curve in a 3-dimensional space; for zero black-hole spin this deformation is curve-shortening that has been extensively studied by mathematicians. The evolution features competing effects of loop growth by the superradiant extraction of the black-hole spin energy, and loop decay by the friction of the moving string against the horizon. A self-intersection of an auxiliary curve corresponds to a capture by the black hole of a new string segment and thus an addition of a new captured loop. Possible asymptotic states of such evolution are shown to be strong emitters of gravitational waves. Whether reconnections prevent reaching the asymptotic states remains to be explored. Additionally, the orbit's shape also evolves due to an emission of gravitational waves, and a recoil of the black hole that changes the orbit and likely leads to self-intersections. \u0000We argue that for a significant range of the dimensionless tension $mu$, string loops are captured by supermassive black holes at the centers of galaxies. This strongly motivates further study of interaction between string loops and black holes, especially the influence of this process on the black hole spindown and on the production of gravitational waves by strings created in galactic nuclei. We also discuss potential loop captures by primordial black holes.","PeriodicalId":8437,"journal":{"name":"arXiv: High Energy Astrophysical Phenomena","volume":"34 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78150902","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: 7