We propose different estimators to probe the epoch of reionization (EoR) intergalactic medium (IGM) using the dispersion measure (${rm DM}$) of the FRBs. We consider three different reionization histories which we can distinguish with a total of $lesssim 1000$ ${rm DM}$ measurements during EoR if their redshifts are known. We note that the redshift derivatives of ${rm DM}$ are also directly sensitive to the reionization history. The major point of this work is exploring the variance in the ${rm DM}$ measurements and the information encoded in them. We find that the all-sky average $overline{{rm DM}}(z)$ gets biased from the LoS fluctuations in the ${rm DM}$ measurements introduced by the ionization of IGM during EoR. We find that the ratio $sigma_{rm DM}/overline{{rm DM}}$ depends directly on the ionization bubble sizes as well as the reionization history. On the other hand, we also find that angular variance (coined as $structure$ $function$) of ${rm DM}$ encodes the information about the duration of reionization and the typical bubble sizes as well. We establish the usefulness of variances in ${rm DM}$ using toy models of reionization and later verify it with the realistic reionization simulations.
{"title":"Asking Fast Radio Bursts (FRBs) for More than Reionization History","authors":"Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar","doi":"arxiv-2409.03255","DOIUrl":"https://doi.org/arxiv-2409.03255","url":null,"abstract":"We propose different estimators to probe the epoch of reionization (EoR)\u0000intergalactic medium (IGM) using the dispersion measure (${rm DM}$) of the\u0000FRBs. We consider three different reionization histories which we can\u0000distinguish with a total of $lesssim 1000$ ${rm DM}$ measurements during EoR\u0000if their redshifts are known. We note that the redshift derivatives of ${rm\u0000DM}$ are also directly sensitive to the reionization history. The major point\u0000of this work is exploring the variance in the ${rm DM}$ measurements and the\u0000information encoded in them. We find that the all-sky average $overline{{rm\u0000DM}}(z)$ gets biased from the LoS fluctuations in the ${rm DM}$ measurements\u0000introduced by the ionization of IGM during EoR. We find that the ratio\u0000$sigma_{rm DM}/overline{{rm DM}}$ depends directly on the ionization bubble\u0000sizes as well as the reionization history. On the other hand, we also find that\u0000angular variance (coined as $structure$ $function$) of ${rm DM}$ encodes the\u0000information about the duration of reionization and the typical bubble sizes as\u0000well. We establish the usefulness of variances in ${rm DM}$ using toy models\u0000of reionization and later verify it with the realistic reionization\u0000simulations.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206588","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}
We describe a novel splitting approach to numerical relativistic magnetohydrodynamics (RMHD) designed to expand its applicability to the domain of ultra-high magnetisation (high-$sigma$). In this approach, the electromagnetic field is split into the force-free component and its perturbation due to the plasma inertia. Accordingly, the system of RMHD equations is extended to include the subsystem of force-free degenerate electrodynamics and the subsystem governing the plasma dynamics and the perturbation of the force-free field. The combined system of conservation laws is integrated simultaneously, to which aim various numerical techniques can be used, and the force-free field is recombined with its perturbation at the end of every timestep. To explore the potential of this splitting approach, we combined it with a 3rd-order WENO method, and carried out a variety of 1D and 2D test simulations. The simulations confirm the robustness of the splitting method in the high-$sigma$ regime, and also show that it remains accurate in the low-$sigma$ regime, all the way down to $sigma$ = 0. Thus, the method can be used for simulating complex astrophysical flows involving a wide range of physical parameters. The numerical resistivity of the code obeys a simple ansatz and allows fast magnetic reconnection in the plasmoid-dominated regime. The results of simulations involving thin and long current sheets agree very well with the theory of resistive magnetic reconnection.
{"title":"A splitting method for numerical relativistic magnetohydrodynamics","authors":"Serguei Komissarov, David Phillips","doi":"arxiv-2409.03637","DOIUrl":"https://doi.org/arxiv-2409.03637","url":null,"abstract":"We describe a novel splitting approach to numerical relativistic\u0000magnetohydrodynamics (RMHD) designed to expand its applicability to the domain\u0000of ultra-high magnetisation (high-$sigma$). In this approach, the\u0000electromagnetic field is split into the force-free component and its\u0000perturbation due to the plasma inertia. Accordingly, the system of RMHD\u0000equations is extended to include the subsystem of force-free degenerate\u0000electrodynamics and the subsystem governing the plasma dynamics and the\u0000perturbation of the force-free field. The combined system of conservation laws\u0000is integrated simultaneously, to which aim various numerical techniques can be\u0000used, and the force-free field is recombined with its perturbation at the end\u0000of every timestep. To explore the potential of this splitting approach, we\u0000combined it with a 3rd-order WENO method, and carried out a variety of 1D and\u00002D test simulations. The simulations confirm the robustness of the splitting\u0000method in the high-$sigma$ regime, and also show that it remains accurate in\u0000the low-$sigma$ regime, all the way down to $sigma$ = 0. Thus, the method can\u0000be used for simulating complex astrophysical flows involving a wide range of\u0000physical parameters. The numerical resistivity of the code obeys a simple\u0000ansatz and allows fast magnetic reconnection in the plasmoid-dominated regime.\u0000The results of simulations involving thin and long current sheets agree very\u0000well with the theory of resistive magnetic reconnection.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206583","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}
Qiliang Fang, Takashi J. Moriya, Lucía Ferrari, Keiichi Maeda, Gaston Folatelli, Keila Y. Ertini, Hanindyo Kuncarayakti, Jennifer E. Andrews, Tatsuya Matsumoto
SN 2023ixf is one of the most well-observed core-collapse supernova in recent decades, yet there is inconsistency in the inferred zero-age-main-sequence (ZAMS) mass $M_{rm ZAMS}$ of its progenitor. Direct observations of the pre-SN red supergiant (RSG) estimate $M_{rm ZAMS}$ spanning widely from 11 to 18 $M_{rm odot}$. Additional constraints, including host environment and the pulsation of its progenitor RSG, suggest a massive progenitor with $M_{rm ZAMS}$ > 17 $M_{rm odot}$. However, the analysis of the properties of supernova, from light curve modeling to late phase spectroscopy, favor a relatively low mass scenario ($M_{rm ZAMS}$ < 15 $M_{rm odot}$). In this work, we conduct systematic analysis of SN 2023ixf, from the RSG progenitor, plateau phase light curve to late phase spectroscopy. Using MESA+STELLA to simulate the RSG progenitor and their explosions, we find that, despite the ZAMS mass of the RSG models being varied from 12.0 to 17.5 $M_{rm odot}$, they can produce light curves that well match with SN 2023ixf if the envelope mass and the explosion energy are allowed to vary. Using late phase spectroscopy as independent measurement, the oxygen emission line [O I] suggests the ZAMS is intermediate massive (~16.0 $M_{rm odot}$), and the relatively weak H$alpha$ emission line indicates the hydrogen envelope has been partially removed before the explosion. By incorporating the velocity structure derived from the light curve modeling into an axisymmetric model, we successfully generated [O I] line profiles that are consistent with the [O I] line observed in late phase spectroscopy of SN 2023ixf. Bringing these analyses together, we conclude that SN 2023ixf is the aspherical explosion of an intermediate massive star ($M_{rm ZAMS}$ = 15-16 $M_{rm odot}$) with the hydrogen envelope being partially stripped to 4-5 $M_{rm odot}$ prior to its explosion.
{"title":"Diversity in hydrogen-rich envelope mass of type II supernovae (II): SN 2023ixf as explosion of partially-stripped intermediate massive star","authors":"Qiliang Fang, Takashi J. Moriya, Lucía Ferrari, Keiichi Maeda, Gaston Folatelli, Keila Y. Ertini, Hanindyo Kuncarayakti, Jennifer E. Andrews, Tatsuya Matsumoto","doi":"arxiv-2409.03540","DOIUrl":"https://doi.org/arxiv-2409.03540","url":null,"abstract":"SN 2023ixf is one of the most well-observed core-collapse supernova in recent\u0000decades, yet there is inconsistency in the inferred zero-age-main-sequence\u0000(ZAMS) mass $M_{rm ZAMS}$ of its progenitor. Direct observations of the pre-SN\u0000red supergiant (RSG) estimate $M_{rm ZAMS}$ spanning widely from 11 to 18\u0000$M_{rm odot}$. Additional constraints, including host environment and the\u0000pulsation of its progenitor RSG, suggest a massive progenitor with $M_{rm\u0000ZAMS}$ > 17 $M_{rm odot}$. However, the analysis of the properties of\u0000supernova, from light curve modeling to late phase spectroscopy, favor a\u0000relatively low mass scenario ($M_{rm ZAMS}$ < 15 $M_{rm odot}$). In this\u0000work, we conduct systematic analysis of SN 2023ixf, from the RSG progenitor,\u0000plateau phase light curve to late phase spectroscopy. Using MESA+STELLA to\u0000simulate the RSG progenitor and their explosions, we find that, despite the\u0000ZAMS mass of the RSG models being varied from 12.0 to 17.5 $M_{rm odot}$,\u0000they can produce light curves that well match with SN 2023ixf if the envelope\u0000mass and the explosion energy are allowed to vary. Using late phase\u0000spectroscopy as independent measurement, the oxygen emission line [O I]\u0000suggests the ZAMS is intermediate massive (~16.0 $M_{rm odot}$), and the\u0000relatively weak H$alpha$ emission line indicates the hydrogen envelope has\u0000been partially removed before the explosion. By incorporating the velocity\u0000structure derived from the light curve modeling into an axisymmetric model, we\u0000successfully generated [O I] line profiles that are consistent with the [O I]\u0000line observed in late phase spectroscopy of SN 2023ixf. Bringing these analyses\u0000together, we conclude that SN 2023ixf is the aspherical explosion of an\u0000intermediate massive star ($M_{rm ZAMS}$ = 15-16 $M_{rm odot}$) with the\u0000hydrogen envelope being partially stripped to 4-5 $M_{rm odot}$ prior to its\u0000explosion.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206613","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}
Broad absorption line (BAL) outflows are commonly detected in active galactic nuclei (AGN), but their driving mechanism remains poorly constrained. Here we investigate whether radiation pressure on dust can adequately explain the BAL phenomenon observed in quasars. In the framework of our AGN radiative dusty feedback scenario, we show that dust-driven outflows can reach BAL wind-like velocities ($v sim 10^4$ km/s) on galactic scales ($r lesssim 1$ kpc). This is consistent with recent observations indicating that BAL acceleration typically occurs on scales of $sim 10$ pc, and that the majority of BAL outflows are located at galactocentric radii greater than $sim 100$ pc. We derive the outflow radial velocity profile and compute the associated outflow momentum rate and kinetic power, which are found to be in agreement with the outflow energetics measured in BAL quasars. Therefore radiation pressure on dust may account for the observed BAL outflow dynamics and energetics. Furthermore, we consider BAL clouds/clumps (leading to a clumpy BAL flow characterised by a wide range of outflowing velocities), and we analyse how the resulting covering factors affect the shape of the absorption line profiles. We conclude that dust-driven BAL outflows may provide a significant contribution to AGN feedback on galactic scales.
在活动星系核（AGN）中通常能探测到宽吸收线（BAL）外流，但对其驱动机制的研究还很不够。在这里，我们研究了尘埃上的辐射压力能否充分解释类星体中观测到的宽吸收线现象。在我们的AGN辐射尘埃反馈情景框架中，我们表明尘埃驱动的外流可以在星系尺度（$r lesssim 1$ kpc）上达到类似BAL风的速度（$v sim 10^4$ km/s）。这与最近的观测结果是一致的，这些观测结果表明BAL加速通常发生在10^4^km/s的尺度上，而且大多数BAL外流位于银河系半径大于100^4^km/s的地方。我们对流出的径向速度剖面进行了分析，并计算了相关的流出动量率和动能，发现它们与在BAL类星体中测得的流出能量是一致的。因此，尘埃上的辐射压力可能是观测到的 BAL 外流动力学和能量学的原因。此外，我们还考虑了 BAL 云/团块（导致以大范围外流速度为特征的团状 BAL 流），并分析了由此产生的覆盖因素如何影响吸收线剖面的形状。我们的结论是，尘埃驱动的 BAL 外流可能会对银河尺度上的 AGN 反馈做出重要贡献。
{"title":"Are BAL outflows powered by radiation pressure on dust?","authors":"W. Ishibashi, A. C. Fabian, P. C. Hewett","doi":"arxiv-2409.03842","DOIUrl":"https://doi.org/arxiv-2409.03842","url":null,"abstract":"Broad absorption line (BAL) outflows are commonly detected in active galactic\u0000nuclei (AGN), but their driving mechanism remains poorly constrained. Here we\u0000investigate whether radiation pressure on dust can adequately explain the BAL\u0000phenomenon observed in quasars. In the framework of our AGN radiative dusty\u0000feedback scenario, we show that dust-driven outflows can reach BAL wind-like\u0000velocities ($v sim 10^4$ km/s) on galactic scales ($r lesssim 1$ kpc). This\u0000is consistent with recent observations indicating that BAL acceleration\u0000typically occurs on scales of $sim 10$ pc, and that the majority of BAL\u0000outflows are located at galactocentric radii greater than $sim 100$ pc. We\u0000derive the outflow radial velocity profile and compute the associated outflow\u0000momentum rate and kinetic power, which are found to be in agreement with the\u0000outflow energetics measured in BAL quasars. Therefore radiation pressure on\u0000dust may account for the observed BAL outflow dynamics and energetics.\u0000Furthermore, we consider BAL clouds/clumps (leading to a clumpy BAL flow\u0000characterised by a wide range of outflowing velocities), and we analyse how the\u0000resulting covering factors affect the shape of the absorption line profiles. We\u0000conclude that dust-driven BAL outflows may provide a significant contribution\u0000to AGN feedback on galactic scales.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206582","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}
N. A. Rakotondrainibe, V. Buat, D. Turpin, D. Dornic, E. LeFloc'h, S. D. Vergani, S. Basa
Gamma-ray burst (GRB) afterglows are powerful probes for studying the different properties of their host galaxies (e.g., the interstellar dust) at all redshifts. By fitting their spectral energy distribution (SED) over a large range of wavelengths, we can gain direct insights into the properties of the interstellar dust by studying the extinction curves. Unlike the dust extinction templates, such as the average Milky Way (MW) or the Small and Large Magellanic Cloud (SMC and LMC), the extinction curves of galaxies outside the Local Group exhibit deviation from these laws. Altogether, X-ray and gamma-ray satellites as well as ground-based telescopes, such as Neil Gehrels Swift Observatory (Swift) and Gamma-Ray Optical and Near-Infrared Detector (GROND), provide measurements of the afterglows from the X-ray to the NIR, which can be used to extract information on dust extinction curves along their lines of sight. The study presented in this paper undertakes such a photometric study, comprising a preparatory work for the SVOM mission and its ground-based follow-up telescope COLIBRI. We propose a simple parameterization of the dust extinction curve of GRB host galaxies. Our model is based on a power law form with the addition of a Loretzian-like Drude profile with two parameters: the extinction slope, $gamma$, and the 2175 $AA$ bump amplitude, $E_rm{b}$. Using the seven GROND filter bands, we tested our dust extinction model and explored the parameter space in extinction and redshift by fitting SEDs of simplified simulations of GRB afterglow spectra based on different extinction curve templates. From a final sample of 10 real Swift/GROND extinguished GRBs, we determined the quantities of the dust extinction in their host and measured their extinction curves. The measured average extinction curve is equivalent to a quasi-featureless in-between SMC-LMC template.
伽马射线暴（GRB）余辉是研究所有红移下宿主星系（如星际尘埃）不同性质的强大探测器。通过在更大的波长范围内拟合它们的光谱能量分布（SED），我们可以通过研究消光曲线直接了解星际尘埃的性质。与平均银河系（MW）或小麦哲伦云和大麦哲伦云（SMC 和 LMC）等尘埃消光模板不同，本星系群以外的星系的消光曲线偏离了这些规律。X 射线和伽马射线卫星以及地面望远镜，如 Neil Gehrels Swift 天文台（Swift）和伽马射线光学和近红外探测器（GROND），都提供了从 X 射线到近红外的余辉测量数据，可用于提取沿其视线的尘埃消光曲线信息。本文介绍的研究就是进行这样的测光研究，包括为 SVOM 任务及其地面跟踪望远镜 COLIBRI 所做的准备工作。我们提出了一个简单的GRB宿主星系尘埃消光曲线参数化模型。我们的模型是基于幂律形式的，并增加了一个类似于洛尔兹的德鲁德曲线（Drude profile），其中有两个参数：消光斜率（gamma）和2175 $AA$ 碰撞幅度（E_rm{b}$）。利用七个GROND滤波波段，我们测试了我们的尘埃消光模型，并通过基于不同消光曲线模板的GRB余辉光谱简化模拟的SED拟合，探索了消光和红移的参数空间。我们从最终的10个真实的Swift/GROND熄灭GRB样本中，确定了它们宿主的尘埃消光量，并测量了它们的消光曲线。测得的平均消光曲线相当于介于SMC-LMC模板之间的无水汽特征曲线。
{"title":"A simple model of dust extinction in gamma-ray burst host galaxies","authors":"N. A. Rakotondrainibe, V. Buat, D. Turpin, D. Dornic, E. LeFloc'h, S. D. Vergani, S. Basa","doi":"arxiv-2409.03570","DOIUrl":"https://doi.org/arxiv-2409.03570","url":null,"abstract":"Gamma-ray burst (GRB) afterglows are powerful probes for studying the\u0000different properties of their host galaxies (e.g., the interstellar dust) at\u0000all redshifts. By fitting their spectral energy distribution (SED) over a large\u0000range of wavelengths, we can gain direct insights into the properties of the\u0000interstellar dust by studying the extinction curves. Unlike the dust extinction\u0000templates, such as the average Milky Way (MW) or the Small and Large Magellanic\u0000Cloud (SMC and LMC), the extinction curves of galaxies outside the Local Group\u0000exhibit deviation from these laws. Altogether, X-ray and gamma-ray satellites\u0000as well as ground-based telescopes, such as Neil Gehrels Swift Observatory\u0000(Swift) and Gamma-Ray Optical and Near-Infrared Detector (GROND), provide\u0000measurements of the afterglows from the X-ray to the NIR, which can be used to\u0000extract information on dust extinction curves along their lines of sight. The\u0000study presented in this paper undertakes such a photometric study, comprising a\u0000preparatory work for the SVOM mission and its ground-based follow-up telescope\u0000COLIBRI. We propose a simple parameterization of the dust extinction curve of\u0000GRB host galaxies. Our model is based on a power law form with the addition of\u0000a Loretzian-like Drude profile with two parameters: the extinction slope,\u0000$gamma$, and the 2175 $AA$ bump amplitude, $E_rm{b}$. Using the seven GROND\u0000filter bands, we tested our dust extinction model and explored the parameter\u0000space in extinction and redshift by fitting SEDs of simplified simulations of\u0000GRB afterglow spectra based on different extinction curve templates. From a\u0000final sample of 10 real Swift/GROND extinguished GRBs, we determined the\u0000quantities of the dust extinction in their host and measured their extinction\u0000curves. The measured average extinction curve is equivalent to a\u0000quasi-featureless in-between SMC-LMC template.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206591","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}
Magnetic field evolution of neutron stars is a long-standing debate. The rate of magnetic field decay for isolated, non-accreting neutron stars can be quantified by measuring the negative second derivative of the spin period. Alternatively, this rate can be estimated by observing an excess of thermal emission with respect to the standard cooling without additional heating mechanisms involved. One of the nearby cooling isolated neutron stars -- RX J0720.4-3125, -- offers a unique opportunity to probe the field decay as for this source there are independent measurements of the surface X-ray luminosity, the second spin period derivative, and magnetic field. We demonstrate that the evolution rate of the spin period derivative is in correspondence with the rate of dissipation of magnetic energy of the dipolar field if a significant part of the released energy is emitted in X-rays. The instantaneous time scale for the magnetic field decay is $sim 10^4$ years.
中子星的磁场演化是一个长期争论的问题。通过测量自旋周期的负二阶导数，可以量化孤立的、不产生磁场的中子星的磁场衰变速率。或者，在不涉及额外加热机制的情况下，通过观测相对于标准冷却的过量热辐射，也可以估算出这一速率。附近一颗正在冷却的孤立中子星--RXJ0720.4-3125--为探测磁场衰变提供了一个独特的机会，因为这个来源有独立的表面X射线光度、自旋周期负二阶导数和磁场测量数据。我们证明了自旋周期导数的变化率与双极性磁场磁能的耗散率是一致的，如果释放的能量有很大一部分是以 X 射线形式发射出来的话。磁场衰减的瞬时时间尺度为 $sim 10^4$ 年。
{"title":"Indication of rapid magnetic field decay in X-ray Dim Isolated Neutron Star RX J0720.4-3125","authors":"Andrei P. Igoshev, Sergei B. Popov","doi":"arxiv-2409.03573","DOIUrl":"https://doi.org/arxiv-2409.03573","url":null,"abstract":"Magnetic field evolution of neutron stars is a long-standing debate. The rate\u0000of magnetic field decay for isolated, non-accreting neutron stars can be\u0000quantified by measuring the negative second derivative of the spin period.\u0000Alternatively, this rate can be estimated by observing an excess of thermal\u0000emission with respect to the standard cooling without additional heating\u0000mechanisms involved. One of the nearby cooling isolated neutron stars -- RX\u0000J0720.4-3125, -- offers a unique opportunity to probe the field decay as for\u0000this source there are independent measurements of the surface X-ray luminosity,\u0000the second spin period derivative, and magnetic field. We demonstrate that the\u0000evolution rate of the spin period derivative is in correspondence with the rate\u0000of dissipation of magnetic energy of the dipolar field if a significant part of\u0000the released energy is emitted in X-rays. The instantaneous time scale for the\u0000magnetic field decay is $sim 10^4$ years.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206586","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}
Adi Foord, Francesca Civano, Julia M. Comerford, Martin Elvis, Giuseppina Fabbiano, Tingting Liu, Elisabeta Lusso, Stefano Marchesi, Mar Mezcua, Francisco Muller-Sanchez, Rebecca Nevin, Kristina Nyland
We present a multi-wavelength analysis of MCG+11-11-032, a nearby AGN with the unique classification of both a binary and a dual AGN candidate. With new Chandra observations we aim to resolve any dual AGN system via imaging data, and search for signs of a binary AGN via analysis of the X-ray spectrum. Analyzing the Chandra spectrum, we find no evidence of previously suggested double-peaked Fe K$alpha$ lines; the spectrum is instead best fit by an absorbed powerlaw with a single Fe K$alpha$ line, as well as an additional line centered at $approx$7.5 keV. The Chandra observation reveals faint, soft, and extended X-ray emission, possibly linked to low-level nuclear outflows. Further analysis shows evidence for a compact, hard source -- MCG+11-11-032 X2 -- located 3.27'' from the primary AGN. Modeling MCG+11-11-032 X2 as a compact source, we find that it is relatively luminous ($L_{text{2$-$10 keV}} = 1.52_{-0.48}^{+0.96}times 10^{41}$ erg s$^{-1}$), and the location is coincident with an compact and off-nuclear source resolved in Hubble Space Telescope infrared (F105W) and ultraviolet (F621M, F547M) bands. Pairing our X-ray results with a 144 MHz radio detection at the host galaxy location, we observe X-ray and radio properties similar to those of ESO 243-49 HLX-1, suggesting that MCG+11-11-032 X2 may be a hyper-luminous X-ray source. This detection with Chandra highlights the importance of a high-resolution X-ray imager, and how previous binary AGN candidates detected with large-aperture instruments benefit from high-resolution follow-up. Future spatially resolved optical spectra, and deeper X-ray observations, can better constrain the origin of MCG+11-11-032 X2.
{"title":"Chandra Discovery of a Candidate Hyper-Luminous X-ray Source in MCG+11-11-032","authors":"Adi Foord, Francesca Civano, Julia M. Comerford, Martin Elvis, Giuseppina Fabbiano, Tingting Liu, Elisabeta Lusso, Stefano Marchesi, Mar Mezcua, Francisco Muller-Sanchez, Rebecca Nevin, Kristina Nyland","doi":"arxiv-2409.03839","DOIUrl":"https://doi.org/arxiv-2409.03839","url":null,"abstract":"We present a multi-wavelength analysis of MCG+11-11-032, a nearby AGN with\u0000the unique classification of both a binary and a dual AGN candidate. With new\u0000Chandra observations we aim to resolve any dual AGN system via imaging data,\u0000and search for signs of a binary AGN via analysis of the X-ray spectrum.\u0000Analyzing the Chandra spectrum, we find no evidence of previously suggested\u0000double-peaked Fe K$alpha$ lines; the spectrum is instead best fit by an\u0000absorbed powerlaw with a single Fe K$alpha$ line, as well as an additional\u0000line centered at $approx$7.5 keV. The Chandra observation reveals faint, soft,\u0000and extended X-ray emission, possibly linked to low-level nuclear outflows.\u0000Further analysis shows evidence for a compact, hard source -- MCG+11-11-032 X2\u0000-- located 3.27'' from the primary AGN. Modeling MCG+11-11-032 X2 as a compact\u0000source, we find that it is relatively luminous ($L_{text{2$-$10 keV}} =\u00001.52_{-0.48}^{+0.96}times 10^{41}$ erg s$^{-1}$), and the location is\u0000coincident with an compact and off-nuclear source resolved in Hubble Space\u0000Telescope infrared (F105W) and ultraviolet (F621M, F547M) bands. Pairing our\u0000X-ray results with a 144 MHz radio detection at the host galaxy location, we\u0000observe X-ray and radio properties similar to those of ESO 243-49 HLX-1,\u0000suggesting that MCG+11-11-032 X2 may be a hyper-luminous X-ray source. This\u0000detection with Chandra highlights the importance of a high-resolution X-ray\u0000imager, and how previous binary AGN candidates detected with large-aperture\u0000instruments benefit from high-resolution follow-up. Future spatially resolved\u0000optical spectra, and deeper X-ray observations, can better constrain the origin\u0000of MCG+11-11-032 X2.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206565","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}
This study investigates the detectability of intermediate-mass black holes (IMBHs) within the mass range $10^2-10^5$ solar masses in the globular star clusters of NGC 1399 at a frequency of 300.00 MHz. Employing the theoretical Bondi accretion model and the empirical fundamental plane of black hole accretion, we estimate IMBH masses based on bolometric luminosity and X-ray/radio luminosities, respectively. By simulating a 3-hour observation of 77 globular cluster candidates using the Square Kilometer Array, we identify radio detection benchmarks indicative of accretion onto IMBHs. Our results show that IMBHs inside the globular star clusters located in NGC 1399 are indeed detectable, with the Bondi accretion model providing IMBH mass estimates ranging from $2.93 times 10^{3.0pm 0.39}$ to $7.43 times 10^{4.0 pm 0.39}$ solar masses, and the empirical fundamental-plane relation suggesting IMBH mass estimation with $3.41times 10^{5.0 pm 0.96}$ solar masses. These findings highlight the presence and detectability of IMBHs in globular clusters, offering insights into their role as precursors to supermassive black holes and enriching our understanding of black hole formation and evolution in astrophysical environments.
{"title":"Prospects for Revealing Intermediate-Mass Black Holes in NGC 1399 using SKA","authors":"B. Karimi, P. Barmby, S. Abbassi","doi":"arxiv-2409.02893","DOIUrl":"https://doi.org/arxiv-2409.02893","url":null,"abstract":"This study investigates the detectability of intermediate-mass black holes\u0000(IMBHs) within the mass range $10^2-10^5$ solar masses in the globular star\u0000clusters of NGC 1399 at a frequency of 300.00 MHz. Employing the theoretical\u0000Bondi accretion model and the empirical fundamental plane of black hole\u0000accretion, we estimate IMBH masses based on bolometric luminosity and\u0000X-ray/radio luminosities, respectively. By simulating a 3-hour observation of\u000077 globular cluster candidates using the Square Kilometer Array, we identify\u0000radio detection benchmarks indicative of accretion onto IMBHs. Our results show\u0000that IMBHs inside the globular star clusters located in NGC 1399 are indeed\u0000detectable, with the Bondi accretion model providing IMBH mass estimates\u0000ranging from $2.93 times 10^{3.0pm 0.39}$ to $7.43 times 10^{4.0 pm 0.39}$\u0000solar masses, and the empirical fundamental-plane relation suggesting IMBH mass\u0000estimation with $3.41times 10^{5.0 pm 0.96}$ solar masses. These findings\u0000highlight the presence and detectability of IMBHs in globular clusters,\u0000offering insights into their role as precursors to supermassive black holes and\u0000enriching our understanding of black hole formation and evolution in\u0000astrophysical environments.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206614","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}
The extraordinary gamma-ray burst GRB 221009A provides a great opportunity to investigate the enigmatic origin and evolution of GRBs. However, the complexity of the observations associated with this GRB provides significant challenges to develop a theoretical modeling in a coherent framework. In this paper, we present a theoretical interpretation of the GRB 221009A afterglow within the relativistic fireball scenario, aiming to describe the broad-band dataset with a consistent model evolution. We find that the adiabatic fireball evolution in the slow-cooling regime provides a viable scenario in good agreement with observations. Crucial to our analysis is the set of simultaneous GeV and TeV gamma-ray data obtained by AGILE and LHAASO during the early afterglow phases. Having successfully modelled as inverse Compton emission the high-energy spectral and lightcurve properties of the afterglow up to $10^4$ s, we extend our model to later times when also optical and X-ray data are available. This approach results in a coherent physical framework that successfully describes all observed properties of the afterglow up to very late times, approximately $10^6$ s. Our model requires time-variable microphysical parameters, with a moderately increasing efficiency $varepsilon_e$ of a few percent for transferring the shock energy to radiating particles, and a decreasing efficiency for magnetic field generation $varepsilon_B$ in the range $10^{-5}$ to $10^{-7}$. Fitting the detailed multi-frequency spectral data across the afterglow provides a unique test of our model.
非同寻常的伽马射线暴GRB 221009A为研究伽马射线暴的神秘起源和演变提供了一个绝佳的机会。然而，与这一伽马射线暴相关的观测数据的复杂性为在一个连贯的框架内建立理论模型带来了巨大的挑战。在本文中，我们提出了在相对论火球情景下对GRB 221009A余辉的理论解释，旨在用一致的模型演化来描述宽波段数据集。我们发现，绝热火球在慢冷却机制下的演化提供了一个可行的方案，与观测结果非常吻合。在成功地将 10^4$ 秒以内的余辉的高能谱和光曲线特性模拟为反康普顿发射之后，我们将模型扩展到了光学和 X 射线数据也可用的后期。我们的模型需要随时间变化的微观物理参数，将冲击能量转移到辐射粒子的效率$varepsilon_e$略微增加了几个百分点，而磁场产生的效率$varepsilon_B$则在$10^{-5}$到$10^{-7}$范围内下降了。拟合整个余辉的详细多频谱数据为我们的模型提供了一个独特的检验。
{"title":"Theoretical modelling of the exceptional GRB 221009A afterglow","authors":"L. Foffano, M. Tavani, G. Piano","doi":"arxiv-2409.02859","DOIUrl":"https://doi.org/arxiv-2409.02859","url":null,"abstract":"The extraordinary gamma-ray burst GRB 221009A provides a great opportunity to\u0000investigate the enigmatic origin and evolution of GRBs. However, the complexity\u0000of the observations associated with this GRB provides significant challenges to\u0000develop a theoretical modeling in a coherent framework. In this paper, we\u0000present a theoretical interpretation of the GRB 221009A afterglow within the\u0000relativistic fireball scenario, aiming to describe the broad-band dataset with\u0000a consistent model evolution. We find that the adiabatic fireball evolution in\u0000the slow-cooling regime provides a viable scenario in good agreement with\u0000observations. Crucial to our analysis is the set of simultaneous GeV and TeV\u0000gamma-ray data obtained by AGILE and LHAASO during the early afterglow phases.\u0000Having successfully modelled as inverse Compton emission the high-energy\u0000spectral and lightcurve properties of the afterglow up to $10^4$ s, we extend\u0000our model to later times when also optical and X-ray data are available. This\u0000approach results in a coherent physical framework that successfully describes\u0000all observed properties of the afterglow up to very late times, approximately\u0000$10^6$ s. Our model requires time-variable microphysical parameters, with a\u0000moderately increasing efficiency $varepsilon_e$ of a few percent for\u0000transferring the shock energy to radiating particles, and a decreasing\u0000efficiency for magnetic field generation $varepsilon_B$ in the range $10^{-5}$\u0000to $10^{-7}$. Fitting the detailed multi-frequency spectral data across the\u0000afterglow provides a unique test of our model.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206589","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}
Noam SokerTechnion, Israel, Dmitry ShishkinTechnion, Israel
We identify an S-shaped main-jet axis in the Vela core-collapse supernova (CCSN) remnant (CCSNR) that we attribute to a pair of precessing jets, one of the tens of pairs of jets that exploded the progenitor of Vela according to the jittering jets explosion mechanism (JJEM). A main-jet axis is a symmetry axis across the CCSNR and through the center. We identify the S-shaped main-jet axis by the high abundance of ejecta elements, oxygen, neon, and magnesium. We bring the number of identified pairs of clumps and ears in Vela to seven, two pairs shaped by the pair of precessing jets that formed the main-jet axis. The pairs and the main-jet axis form the point-symmetric wind-rose structure of Vela. The other five pairs of clumps/ears do not have signatures near the center, only on two opposite sides of the CCSNR. We discuss different possible jet-less shaping mechanisms to form such a point-symmetric morphology and dismiss these processes because they cannot explain the point-symmetric morphology of Vela, the S-shaped high ejecta abundance pattern, and the enormous energy to shape the S-shaped structure. Our findings strongly support the JJEM and further severely challenge the neutrino-driven explosion mechanism.
我们在维拉核心-坍缩超新星（CCSN）残余（CCSNR）中发现了一条S形主喷流轴，我们把它归因于一对前冲喷流，根据抖动喷流爆炸机制（JJEM），这是维拉原生星爆炸的数十对喷流之一。主喷流轴是横跨CCSNR并穿过中心的对称轴。我们通过喷出物元素（氧、氖和镁）的高丰度来识别 S 形主喷流轴。我们将维拉中已确定的成对星团和星耳数量增加到七对，其中两对是由形成主喷气轴的一对前冲喷流形成的。这对喷流和主喷流轴构成了维拉的点对称风玫瑰结构。另外五对团块状/梨状结构在中心附近没有特征，只在CCSNR的两侧有特征。我们讨论了形成这种点对称形态的各种可能的无射流塑造机制，并否定了这些过程，因为它们无法解释维拉的点对称形态、S形高喷出物丰度模式以及塑造S形结构所需的巨大能量。我们的发现有力地支持了JJEM，并进一步有力地挑战了中微子驱动的爆炸机制。
{"title":"The vela supernova remnant: The unique morphological features of jittering jets","authors":"Noam SokerTechnion, Israel, Dmitry ShishkinTechnion, Israel","doi":"arxiv-2409.02626","DOIUrl":"https://doi.org/arxiv-2409.02626","url":null,"abstract":"We identify an S-shaped main-jet axis in the Vela core-collapse supernova\u0000(CCSN) remnant (CCSNR) that we attribute to a pair of precessing jets, one of\u0000the tens of pairs of jets that exploded the progenitor of Vela according to the\u0000jittering jets explosion mechanism (JJEM). A main-jet axis is a symmetry axis\u0000across the CCSNR and through the center. We identify the S-shaped main-jet axis\u0000by the high abundance of ejecta elements, oxygen, neon, and magnesium. We bring\u0000the number of identified pairs of clumps and ears in Vela to seven, two pairs\u0000shaped by the pair of precessing jets that formed the main-jet axis. The pairs\u0000and the main-jet axis form the point-symmetric wind-rose structure of Vela. The\u0000other five pairs of clumps/ears do not have signatures near the center, only on\u0000two opposite sides of the CCSNR. We discuss different possible jet-less shaping\u0000mechanisms to form such a point-symmetric morphology and dismiss these\u0000processes because they cannot explain the point-symmetric morphology of Vela,\u0000the S-shaped high ejecta abundance pattern, and the enormous energy to shape\u0000the S-shaped structure. Our findings strongly support the JJEM and further\u0000severely challenge the neutrino-driven explosion mechanism.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206590","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}
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