arXiv - PHYS - High Energy Astrophysical Phenomena最新文献_第8页

Fast magnetic reconnection in Kerr spacetime 克尔时空中的快速磁再连接

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-09 DOI: arxiv-2409.05434

Zhong-Ying Fan, Yuehang Li, Fan Zhou, Minyong Guo

引用次数: 0

Detection of the Fe K lines from the binary AGN in 4C+37.11 探测来自 4C+37.11 双 AGN 的铁 K 线

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-09 DOI: arxiv-2409.05717

Santanu Mondal, Mousumi Das, K. Rubinur, Karishma Bansal, Aniket Nath, Greg B. Taylor

{"title":"Detection of the Fe K lines from the binary AGN in 4C+37.11","authors":"Santanu Mondal, Mousumi Das, K. Rubinur, Karishma Bansal, Aniket Nath, Greg B. Taylor","doi":"arxiv-2409.05717","DOIUrl":"https://doi.org/arxiv-2409.05717","url":null,"abstract":"We report the discovery of the Fe K line emission at\u0000$sim6.62^{+0.06}_{-0.06}$ keV with a width of $sim0.19^{+0.05}_{-0.05}$ keV\u0000using two epochs of {it Chandra} archival data from the nucleus of the galaxy\u00004C+37.11, which is known to host a binary supermassive black hole (BSMBH)\u0000system where the SMBHs are separated by $sim7$ mas or $sim$ 7pc. Our study\u0000reports the first detection of the Fe K line from a known binary AGN, and has\u0000an F-statistic value of 20.98 and probability $2.47times 10^{-12}$. Stacking\u0000of two spectra reveals another Fe K line component at\u0000$sim7.87^{+0.19}_{-0.09}$ keV. Different model scenarios indicate that the\u0000lines originate from the combined effects of accretion disk emission and\u0000circumnuclear collisionally ionized medium. The observed low column density\u0000favors the gas-poor merger scenario, where the high temperature of the hot\u0000ionized medium may be associated with the shocked gas in the binary merger and\u0000not with star formation activity. The estimated total BSMBH mass and disk\u0000inclination are $sim1.5times10^{10}$ M$_odot$ and $gtrsim75^circ$,\u0000indicating that the BSMBH is probably a high inclination system. The spin\u0000parameter could not be tightly constrained from the present data sets. Our\u0000results draw attention to the fact that detecting the Fe K line emissions from\u0000BSMBHs is important for estimating the individual SMBH masses, and the spins of\u0000the binary SMBHs, as well as exploring their emission regions.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"56 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206850","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: 0

Examining the Relationship Between the Persistent Emission and the Accretion Rate During a Type I X-ray Burst 研究 I 型 X 射线爆发期间的持续发射与吸收率之间的关系

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-09 DOI: arxiv-2409.05737

J. SpeicherCenter for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, D. R. BallantyneCenter for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, P. C. FragileDepartment of Physics & Astronomy, College of Charleston

{"title":"Examining the Relationship Between the Persistent Emission and the Accretion Rate During a Type I X-ray Burst","authors":"J. SpeicherCenter for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, D. R. BallantyneCenter for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, P. C. FragileDepartment of Physics & Astronomy, College of Charleston","doi":"arxiv-2409.05737","DOIUrl":"https://doi.org/arxiv-2409.05737","url":null,"abstract":"The accretion flow onto a neutron star will be impacted due to irradiation by\u0000a Type I X-ray burst. The burst radiation exerts Poynting-Robertson (PR) drag\u0000on the accretion disk, leading to an enhanced mass accretion rate. Observations\u0000of X-ray bursts often find evidence that the normalization of the\u0000disk-generated persistent emission (commonly denoted by the factor $f_a$)\u0000increases during a burst, and changes in $f_a$ have been used to infer the\u0000evolution in the mass accretion rate due to PR drag. Here, we examine this\u0000proposed relationship between $f_a$ and mass accretion rate enhancement using\u0000time-resolved data from simulations of accretion disks impacted by Type I X-ray\u0000bursts. We consider bursts from both spinning and non-spinning neutron stars\u0000and track both the change in accretion rate due to PR grad and the disk\u0000emission spectra during the burst. Regardless of the neutron star spin, we find\u0000that $f_a$ strongly correlates with the disk temperature and only weakly\u0000follows the mass accretion rate (the Pearson correlation coefficients are $leq\u00000.63$ in the latter case). Additionally, heating causes the disk to emit at\u0000higher energies, reducing its contribution to a soft excess. We conclude that\u0000$f_a$ cannot accurately capture the mass accretion rate enhancement and is\u0000rather a tracer of the disk temperature.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206849","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: 0

Origin of the break in the cosmic-ray electron plus positron spectrum at ~ 1 TeV 约 1 TeV 处宇宙射线电子和正电子频谱断裂的起源

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-09 DOI: arxiv-2409.05509

Satyendra Thoudam

{"title":"Origin of the break in the cosmic-ray electron plus positron spectrum at ~ 1 TeV","authors":"Satyendra Thoudam","doi":"arxiv-2409.05509","DOIUrl":"https://doi.org/arxiv-2409.05509","url":null,"abstract":"Recent measurements of the cosmic-ray electron plus positron spectrum by\u0000several experiments have confirmed the presence of a break at $sim,1$ TeV.\u0000The origin of the break is still not clearly understood. In this work, we\u0000explore different possibilities for the origin which include an electron source\u0000spectrum with a broken power-law, a power-law with an exponential or\u0000super-exponential cut-offs and the absence of potential nearby cosmic-ray\u0000sources. Based on the observed electron plus positron data from the DAMPE and\u0000the H.E.S.S experiments, and considering supernova remnants as the main sources\u0000of cosmic rays in the Galaxy, we find statistical evidence in favour of the\u0000scenario with a broken power-law source spectrum with the best-fit source\u0000parameters obtained as $Gamma=2.39$ for the source spectral index, $E_0approx\u00001.6$ TeV for the break energy and $f=1.59times 10^{48}$ ergs for the amount of\u0000supernova kinetic energy injected into cosmic-ray electrons. Such a power-law\u0000break in the spectrum has been predicted for electrons confined inside\u0000supernova remnants after acceleration via diffusive shock acceleration process,\u0000and also indicated by the multi-wavelength study of supernova remnants. All\u0000these evidences have shown that the observed spectral break provides a strong\u0000indication of a direct link between cosmic-ray electrons and their sources. Our\u0000findings further show that electrons must undergo spectral changes while\u0000escaping the source region in order to reconcile the difference between the\u0000spectral index of electrons observed inside supernova remnants and that\u0000obtained from Galactic cosmic-ray propagation studies.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"28 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206544","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: 0

Probing the high frequency variability of NGC 5044: the key to AGN feedback 探测NGC 5044的高频变率：AGN反馈的关键

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-09 DOI: arxiv-2409.06039

Gerrit Schellenberger, Ewan O'Sullivan, Laurence David, Jan Vrtilek, Charles Romero, Glen Petitpas, William Forman, Simona Giacintucci, Mark Gurwell, Christine Jones, Kamlesh Rajpurohit, Francesco Ubertosi, Tiziana Venturi

{"title":"Probing the high frequency variability of NGC 5044: the key to AGN feedback","authors":"Gerrit Schellenberger, Ewan O'Sullivan, Laurence David, Jan Vrtilek, Charles Romero, Glen Petitpas, William Forman, Simona Giacintucci, Mark Gurwell, Christine Jones, Kamlesh Rajpurohit, Francesco Ubertosi, Tiziana Venturi","doi":"arxiv-2409.06039","DOIUrl":"https://doi.org/arxiv-2409.06039","url":null,"abstract":"The active galactic nucleus (AGN) feeding and feedback process in the centers\u0000of galaxy clusters and groups is still not well understood. NGC5044 is the\u0000ideal system in which to study AGN feedback. It hosts the largest known\u0000reservoir of cold gas in any cool-core galaxy group, and features several past\u0000epochs of AGN feedback imprinted as cavities in the X-ray bright intragroup\u0000medium (IGrM), as well as parsec scale jets. We present Submillimeter Array\u0000(SMA) and Karl G. Jansky Very Large Array (VLA) high frequency observations of\u0000NGC5044 to assess the time variability of the mm-waveband emission from the\u0000accretion disk, and quantify the Spectral Energy Distribution (SED) from the\u0000radio to sub-millimeter band. The SED is well described by advection dominated\u0000accretion flow (ADAF) model and self-absorbed jet emission from an aging plasma\u0000with tau ~1kyr. We find a characteristic variability timescale of 150 days,\u0000which constrains the ADAF emission region to about 0.1pc, and the magnetic\u0000field to 4.7mG in the jets and and 870G in the accretion disk. A longer\u0000monitoring/sampling will allow to understand if the underlying process is truly\u0000periodic in nature.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"30 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206848","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: 0

Nature vs Nurture: Three Dimensional MHD Simulations of Misaligned Embedded Circum-Single Disks within an AGN Disk 自然与养育AGN 盘内错位嵌入环单盘的三维 MHD 模拟

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-09 DOI: arxiv-2409.05614

Bhupendra Mishra, Josh Calcino

{"title":"Nature vs Nurture: Three Dimensional MHD Simulations of Misaligned Embedded Circum-Single Disks within an AGN Disk","authors":"Bhupendra Mishra, Josh Calcino","doi":"arxiv-2409.05614","DOIUrl":"https://doi.org/arxiv-2409.05614","url":null,"abstract":"Stellar mass black holes in the disks around active galactic nuclei (AGN) are\u0000promising sources for gravitational wave detections by LIGO/VIRGO. Recent\u0000studies suggest this environment fosters the formation and merger of binary\u0000black holes. Many of these studies often assumed a simple, laminar AGN disk\u0000without magnetic fields or turbulence. In this work, we present the first 3D\u0000magnetohydrodynamical simulations of circum-single disks around isolated and\u0000binary black holes in strongly magnetized, stratified accretion disks with\u0000turbulence driven by magneto-rotational instability. We simulated three\u0000scenarios with varying initial net-vertical magnetic field strengths: weak,\u0000intermediate, and strong. Our results show that weakly magnetized models\u0000produce circum-single disks aligned with the AGN disk's equatorial plane,\u0000similar to past hydrodynamic simulations. However, intermediate and strong\u0000magnetic fields result in randomly misaligned disks, contingent upon the\u0000availability of local ambient angular momentum within turbulent regions. Our\u0000findings emphasize the significant impact of ambient gas in the AGN disk on the\u0000inclination of circum-single disks, linked to magnetically induced\u0000inhomogeneity and angular momentum during disk formation. The presence of\u0000misaligned disks, both in single and binary black hole systems, could have\u0000profound implications for the long-term evolution of black hole spin and the\u0000inclination of the disk at the horizon scale.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"255 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206837","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: 0

Magnetic Interaction in White Dwarf Binaries as Mechanism for Long-Period Radio Transients 作为长周期射电瞬变机制的白矮星双星中的磁相互作用

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-09 DOI: arxiv-2409.05978

Yuanhong Qu, Bing Zhang

引用次数: 0

Low-mass neutron star nucleosynthesis -- stripping scenario 低质量中子星核合成--剥离情景

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-08 DOI: arxiv-2409.05059

A. Yu. IgnatovskiyNIC "Kurchatov Institute"Moscow Institute of Physics and Technology, I. V. PanovNIC "Kurchatov Institute", A. V. YudinNIC "Kurchatov Institute"

引用次数: 0

The influence of the magnetic braking laws on the evolution of persistent and transient low-mass X-ray binaries 磁制动定律对持久和瞬变低质量 X 射线双星演化的影响

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-08 DOI: arxiv-2409.05067

Hao-Ran Yang, Xiang-Dong Li

{"title":"The influence of the magnetic braking laws on the evolution of persistent and transient low-mass X-ray binaries","authors":"Hao-Ran Yang, Xiang-Dong Li","doi":"arxiv-2409.05067","DOIUrl":"https://doi.org/arxiv-2409.05067","url":null,"abstract":"Swift J1858.6$-$0814 (hereafter J1858) is a transient neutron star low-mass\u0000X-ray binary (NS LMXB). There is controversy regarding its donor mass derived\u0000from observations and theoretical calculations. In this paper, we adopt seven\u0000magnetic braking (MB) prescriptions suggested in the literature and different\u0000metallicity $Z$ to simulate the evolution of the LMXB. Our results show that,\u0000employing the MB model proposed by citet{2012ApJ...746...43R} (\"rm12\"), the\u0000Convection And Rotation Boosted (\"carb\") model citep{2019ApJ...886L..31V}, as\u0000well as the Intermediate (\"inter\") and Convection-boosted (\"cboost\") models in\u0000citet{2019MNRAS.483.5595V} can match (part of) the observational parameters of\u0000J1858 well. We then apply our method to other observed LMXBs and find that the\u0000\"rm12\" and \"inter\" MB laws are most promising in explaining transient LMXBs. In\u0000comparison, the simulations with the \"cboost\" and \"carb\" MB laws are more\u0000inclined to reproduce persistent LMXBs and ultra-compact X-ray binaries\u0000(UCXBs), respectively. Our results, though subject to computational and/or\u0000observational bias, show that it is challenging to find a unified MB law that\u0000applies to the NS LMXB sub-populations simultaneously, indicating our lack of\u0000understanding of the true MB law. In addition, we explore the influence of\u0000various MB laws on the magnitude of the bifurcation periods in LMXBs.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206555","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: 0

Multi-epoch UV $-$ X-ray spectral study of NGC 4151 with AstroSat 利用 AstroSat 对 NGC 4151 进行的多波段 UV $-$ X 射线光谱研究

arXiv - PHYS - High Energy Astrophysical Phenomena Pub Date : 2024-09-07 DOI: arxiv-2409.04762

Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra

{"title":"Multi-epoch UV $-$ X-ray spectral study of NGC 4151 with AstroSat","authors":"Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra","doi":"arxiv-2409.04762","DOIUrl":"https://doi.org/arxiv-2409.04762","url":null,"abstract":"We present a multi-wavelength spectral study of NGC 4151 based on five epochs\u0000of simultaneous AstroSat observations in the near ultra-violet (NUV) to hard\u0000X-ray band ($sim 0.005-80$ keV) during $2017 - 2018$. We derived the intrinsic\u0000accretion disk continuum after correcting for internal and Galactic extinction,\u0000contributions from broad and narrow line regions, and emission from the host\u0000galaxy. We found a bluer continuum at brighter UV flux possibly due to\u0000variations in the accretion disk continuum or the UV reddening. We estimated\u0000the intrinsic reddening, $E(B-V) sim 0.4$, using high-resolution HST/STIS\u0000spectrum acquired in March 2000. We used thermal Comptonization, neutral and\u0000ionized absorption, and X-ray reflection to model the X-ray spectra. We\u0000obtained the X-ray absorbing neutral column varying between $N_H sim 1.2-3.4\u0000times 10^{23} cm^{-2}$, which are $sim 100$ times larger than that estimated\u0000from UV extinction, assuming the Galactic dust-to-gas ratio. To reconcile this\u0000discrepancy, we propose two plausible configurations of the obscurer: (a) a\u0000two-zone obscurer consisting of dust-free and dusty regions, divided by the\u0000sublimation radius, or (b) a two-phase obscurer consisting of clumpy, dense\u0000clouds embedded in a low-density medium, resulting in a scenario where a few\u0000dense clouds obscure the compact X-ray source substantially, while the bulk of\u0000UV emission arising from the extended accretion disk passes through the\u0000low-density medium. Furthermore, we find a positive correlation between X-ray\u0000absorption column and $NUV-FUV$ color and UV flux, indicative of enhanced winds\u0000possibly driven by the 'bluer-when-brighter' UV continuum.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"174 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206562","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: 0