Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad323e
Charles E. Romero, Massimo Gaspari, G. Schellenberger, T. Bhandarkar, Mark Devlin, S. Dicker, William Forman, R. Khatri, R. Kraft, L. Di Mascolo, Brian S. Mason, E. Moravec, T. Mroczkowski, P. Nulsen, J. Orlowski-Scherer, K. P. Sarmiento, C. Sarazin, Jonathan Sievers, Yuanyuan Su
{"title":"Erratum: “Inferences from Surface Brightness Fluctuations of Zwicky 3146 via the Sunyaev–Zel’dovich Effect and X-Ray Observations” (2023, ApJ, 951, 41)","authors":"Charles E. Romero, Massimo Gaspari, G. Schellenberger, T. Bhandarkar, Mark Devlin, S. Dicker, William Forman, R. Khatri, R. Kraft, L. Di Mascolo, Brian S. Mason, E. Moravec, T. Mroczkowski, P. Nulsen, J. Orlowski-Scherer, K. P. Sarmiento, C. Sarazin, Jonathan Sievers, Yuanyuan Su","doi":"10.3847/1538-4357/ad323e","DOIUrl":"https://doi.org/10.3847/1538-4357/ad323e","url":null,"abstract":"","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"55 7","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140759333","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad3104
Tsuyoshi Inoue, A. Marcowith, G. Giacinti
Supernova blast wave shock is a very important site of cosmic-ray acceleration. However, the detailed physical process of acceleration, in particular, nonlinear interplay between cosmic-ray streaming and magnetic field amplification, has not been studied under a realistic environment. In this paper, using a unique and novel numerical method, we study cosmic-ray acceleration at supernova blast wave shock propagating in the interstellar medium with well-resolved magnetic field amplification by nonresonant hybrid instability (or Bell instability). We find that the magnetic field is mildly amplified under typical interstellar medium conditions that leads to maximum cosmic-ray energy ≃30 TeV for supernova remnants with age ≃1000 yr consistent with gamma-ray observations. The strength of the amplified magnetic field does not reach the so-called saturation level because the cosmic-ray electric current toward the shock upstream has a finite spatial extent, by which Bell instability cannot experience many e-folding times.
{"title":"Bell Instability–mediated Diffusive Shock Acceleration at Supernova Blast Wave Shock Propagating in the Interstellar Medium","authors":"Tsuyoshi Inoue, A. Marcowith, G. Giacinti","doi":"10.3847/1538-4357/ad3104","DOIUrl":"https://doi.org/10.3847/1538-4357/ad3104","url":null,"abstract":"\u0000 Supernova blast wave shock is a very important site of cosmic-ray acceleration. However, the detailed physical process of acceleration, in particular, nonlinear interplay between cosmic-ray streaming and magnetic field amplification, has not been studied under a realistic environment. In this paper, using a unique and novel numerical method, we study cosmic-ray acceleration at supernova blast wave shock propagating in the interstellar medium with well-resolved magnetic field amplification by nonresonant hybrid instability (or Bell instability). We find that the magnetic field is mildly amplified under typical interstellar medium conditions that leads to maximum cosmic-ray energy ≃30 TeV for supernova remnants with age ≃1000 yr consistent with gamma-ray observations. The strength of the amplified magnetic field does not reach the so-called saturation level because the cosmic-ray electric current toward the shock upstream has a finite spatial extent, by which Bell instability cannot experience many e-folding times.","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"129 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140768910","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad3240
Xin-Zhe 馨哲 Tang 唐, Jing-Kun 景昆 Zhao 赵, Yong 勇 Yang 杨, Xian-Hao 先豪 Ye 叶, G. Zhao 赵, Q. Gao 高
Based on the LAMOST DR9 Medium Resolution Spectra (MRS) catalog, combined with astrometries from Gaia DR3, we conducted an investigation into the substructures in the stellar halo to obtain their chemical and kinematic information. We employed the HDBSCAN algorithm in the (L z , E, L xy ) space for clustering and utilized Mahalanobis distance to merge the clustering results. Ultimately, within the LAMOST DR9 MRS catalog, we identified members of Gaia–Sausage–Enceladus (GSE), Helmi streams, and the high-α disk and in situ halo. Additionally, there are three clusters that cannot be correlated with known substructures. Based on their angular momentum (L z ) characteristics, we have tentatively named two of them High-L z -Cluster-1 (HLC-1) and High-L z -Cluster-2 (HLC-2), both exhibiting high angular momentum (L z ) features. The third cluster, owing to its extremely low L z , is termed the Low-L z -Cluster. Then detailed analysis about those substructures are executed including member stars’ identification and kinematic and chemical distribution. The resulting GSE member stars exhibit a well-defined metallicity distribution function with its peak at [Fe/H] ∼ −1.2, consistent with previous findings, and we found there appear to be some differences in the distribution on the V total–r gal plane between GSE and its included Splash component. Regarding Helmi streams, in the [Mg/Fe]–[Fe/H] plane we detected potential traces of the α-knee phenomenon at [Fe/H] ∼ −1.53. Finally, we tentatively provide the possible origin for the HLC-1 and HLC-2.
基于LAMOST DR9中分辨率光谱（MRS）星表，结合Gaia DR3的天体测量数据，我们对恒星晕中的亚结构进行了研究，以获得它们的化学和运动学信息。我们采用 HDBSCAN 算法在（L z , E, L xy ）空间进行聚类，并利用 Mahalanobis 距离合并聚类结果。最终，在 LAMOST DR9 MRS 星表中，我们发现了 Gaia-Sausage-Enceladus（GSE）、Helmi 流以及高α盘和原位晕的成员。此外，还有三个星团无法与已知的子结构相关联。根据它们的角动量（L z ）特征，我们暂时将其中两个命名为高L z 星团-1（HLC-1）和高L z 星团-2（HLC-2），它们都表现出高角动量（L z ）特征。第三个星团由于其极低的 L z 而被称为低 L z 星团。然后对这些子结构进行详细分析，包括成员星的识别、运动学和化学分布。我们发现，GSE 和其包含的 Splash 部分在 V total-r gal 平面上的分布似乎存在一些差异。关于赫尔米流，在[Mg/Fe]-[Fe/H]平面上，我们在[Fe/H]∼-1.53处探测到了α-膝现象的潜在痕迹。最后，我们初步提出了 HLC-1 和 HLC-2 的可能起源。
{"title":"Visit Nearby Halo Substructures Using LAMOST DR9 MRS Data","authors":"Xin-Zhe 馨哲 Tang 唐, Jing-Kun 景昆 Zhao 赵, Yong 勇 Yang 杨, Xian-Hao 先豪 Ye 叶, G. Zhao 赵, Q. Gao 高","doi":"10.3847/1538-4357/ad3240","DOIUrl":"https://doi.org/10.3847/1538-4357/ad3240","url":null,"abstract":"\u0000 Based on the LAMOST DR9 Medium Resolution Spectra (MRS) catalog, combined with astrometries from Gaia DR3, we conducted an investigation into the substructures in the stellar halo to obtain their chemical and kinematic information. We employed the HDBSCAN algorithm in the (L\u0000 \u0000 z\u0000 , E, L\u0000 \u0000 xy\u0000 ) space for clustering and utilized Mahalanobis distance to merge the clustering results. Ultimately, within the LAMOST DR9 MRS catalog, we identified members of Gaia–Sausage–Enceladus (GSE), Helmi streams, and the high-α disk and in situ halo. Additionally, there are three clusters that cannot be correlated with known substructures. Based on their angular momentum (L\u0000 \u0000 z\u0000 ) characteristics, we have tentatively named two of them High-L\u0000 \u0000 z\u0000 -Cluster-1 (HLC-1) and High-L\u0000 \u0000 z\u0000 -Cluster-2 (HLC-2), both exhibiting high angular momentum (L\u0000 \u0000 z\u0000 ) features. The third cluster, owing to its extremely low L\u0000 \u0000 z\u0000 , is termed the Low-L\u0000 \u0000 z\u0000 -Cluster. Then detailed analysis about those substructures are executed including member stars’ identification and kinematic and chemical distribution. The resulting GSE member stars exhibit a well-defined metallicity distribution function with its peak at [Fe/H] ∼ −1.2, consistent with previous findings, and we found there appear to be some differences in the distribution on the V\u0000 total–r\u0000 gal plane between GSE and its included Splash component. Regarding Helmi streams, in the [Mg/Fe]–[Fe/H] plane we detected potential traces of the α-knee phenomenon at [Fe/H] ∼ −1.53. Finally, we tentatively provide the possible origin for the HLC-1 and HLC-2.","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"146 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140766631","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad320a
A. Belfiore, R. Salvaterra, L. Sidoli, G. Israel, Luigi Stella, Andrea De Luca, S. Mereghetti, P. Esposito, F. Pintore, A. D’Aì, G. R. Rodríguez Castillo, Dominic J. Walton, Felix Fürst, D. Magistrali, A. Wolter, Matteo Imbrogno
We report on the orbit of the binary system powering the most extreme ultraluminous X-ray pulsar known to date: NGC 5907 ULX-1 (hereafter ULX1). ULX1 has been the target of a substantial multi-instrument campaign, mainly in the X-ray band, but no clear counterparts are known in other bands. Although ULX1 is highly variable and pulsations can be transient (regardless of the source flux), the timing data collected so far allow us to investigate the orbit of this system. We find an orbital period Porb=5.7−0.6+0.1days and a projected semi-axis A1=3.1−0.9
我们报告了为迄今已知的最极端超光速X射线脉冲星NGC 5907 ULX-1（以下简称ULX1）提供动力的双星系统的轨道情况。ULX1一直是大量多仪器观测的目标，主要是在X射线波段，但在其他波段还没有明确的对应天体。虽然 ULX1 变率很高，而且脉动可能是瞬时的（与源通量无关），但目前收集到的定时数据允许我们研究这个系统的轨道。我们发现它的轨道周期为 P orb = 5.7 - 0.6 + 0.1 天，投影半轴 A 1 = 3.1 - 0.9 + 0.8 lt - s。最有可能的星历为 P orb = 5.6585(6) 天，A 1 = 3.1(4) LT-s，升交点通过的纪元为 T asc = 57751.37(5) MJD。然而，在 3σ 以内有六个类似的解决方案是可以接受的。我们发现有进一步的迹象表明 ULX1 是一个高质 X 射线双星。这意味着我们是在正面观测它的轨道，倾角为
{"title":"The Orbit of NGC 5907 ULX-1","authors":"A. Belfiore, R. Salvaterra, L. Sidoli, G. Israel, Luigi Stella, Andrea De Luca, S. Mereghetti, P. Esposito, F. Pintore, A. D’Aì, G. R. Rodríguez Castillo, Dominic J. Walton, Felix Fürst, D. Magistrali, A. Wolter, Matteo Imbrogno","doi":"10.3847/1538-4357/ad320a","DOIUrl":"https://doi.org/10.3847/1538-4357/ad320a","url":null,"abstract":"\u0000 <jats:p>We report on the orbit of the binary system powering the most extreme ultraluminous X-ray pulsar known to date: NGC 5907 ULX-1 (hereafter ULX1). ULX1 has been the target of a substantial multi-instrument campaign, mainly in the X-ray band, but no clear counterparts are known in other bands. Although ULX1 is highly variable and pulsations can be transient (regardless of the source flux), the timing data collected so far allow us to investigate the orbit of this system. We find an orbital period <jats:inline-formula>\u0000 <jats:tex-math>\u0000<?CDATA ${P}_{mathrm{orb}}={5.7}_{-0.6}^{+0.1},mathrm{days}$?>\u0000</jats:tex-math>\u0000 <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\">\u0000 <mml:msub>\u0000 <mml:mrow>\u0000 <mml:mi>P</mml:mi>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mi>orb</mml:mi>\u0000 </mml:mrow>\u0000 </mml:msub>\u0000 <mml:mo>=</mml:mo>\u0000 <mml:msubsup>\u0000 <mml:mrow>\u0000 <mml:mn>5.7</mml:mn>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mo>−</mml:mo>\u0000 <mml:mn>0.6</mml:mn>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mo>+</mml:mo>\u0000 <mml:mn>0.1</mml:mn>\u0000 </mml:mrow>\u0000 </mml:msubsup>\u0000 <mml:mspace width=\"0.25em\" />\u0000 <mml:mi>days</mml:mi>\u0000 </mml:math>\u0000 <jats:inline-graphic xmlns:xlink=\"http://www.w3.org/1999/xlink\" xlink:href=\"apjad320aieqn1.gif\" xlink:type=\"simple\" />\u0000 </jats:inline-formula> and a projected semi-axis <jats:inline-formula>\u0000 <jats:tex-math>\u0000<?CDATA ${A}_{1}={3.1}_{-0.9}^{+0.8},mathrm{lt}mbox{--}{rm{s}}$?>\u0000</jats:tex-math>\u0000 <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\">\u0000 <mml:msub>\u0000 <mml:mrow>\u0000 <mml:mi>A</mml:mi>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mn>1</mml:mn>\u0000 </mml:mrow>\u0000 </mml:msub>\u0000 <mml:mo>=</mml:mo>\u0000 <mml:msubsup>\u0000 <mml:mrow>\u0000 <mml:mn>3.1</mml:mn>\u0000 </mml:mrow>\u0000 <mml:mrow>\u0000 <mml:mo>−</mml:mo>\u0000 <mml:mn>0.9</mml:mn>\u0000 </mml:mrow>\u0000 ","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"659 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140787500","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad28c4
M. Yang 杨, Bo 博 Zhang 章, Biwei 碧沩 Jiang 姜, J. Gao 高, Y. Ren 任, Shu 舒 Wang 王, Man I 敏仪 Lam 林, H. Tian 田, Changqing 常青 Luo 罗, B. Chen 陈, Jing 静 Wen 文
The precise definition of the lower mass limit of red supergiant stars (RSGs) is an open question in astrophysics and does not attract much attention. Here, we assemble a spectroscopic evolved cool star sample with 6602 targets, including RSGs, asymptotic giant branch stars, and red giant branch stars, in the Large Magellanic Cloud based on Gaia DR3 and Sloan Digital Sky Survey IV/APOGEE-2. The reference spectrum of each stellar population is built according to the quantile range of relative intensity (1% ∼ 99%). Five different methods, e.g., χ 2, cosine similarity, machine learning (ML), equivalent width, and line ratio, are used in order to separate different stellar populations. ML and χ 2 provide the best and relatively consistent prediction of a certain population. The derived lower limit of the RSG population is able to reach the K s -band tip of the red giant branch (K s ≈12.0 mag), indicating a luminosity as low as about 103.5 L ⊙, which corresponds to a stellar radius of only about 100 R ⊙. Given the mass–luminosity relation of L / L ⊙ = f ( M / M ⊙ ) 3 with f ≈ 15.5 ± 3 and taking into account the mass loss of faint RSGs up to now, the minimal initial mass of the RSG population would be about 6.1 ± 0.4 M ⊙, which is much lower than the traditional threshold of 8 M ⊙ for the massive stars. This is the first spectroscopic evidence, indicating that the lower mass limit of the RSG population is around 6 M ⊙. However, the destinies of such faint RSGs are still elusive and may have a large impact on stellar evolutionary and supernova models.
红超巨星（RSG）质量下限的精确定义是天体物理学中的一个悬而未决的问题，并未引起广泛关注。在这里，我们基于盖亚DR3和斯隆数字巡天IV/APOGEE-2，在大麦哲伦云中建立了一个包含6602个目标的光谱演化冷星样本，其中包括RSGs、渐近巨枝星和红巨枝星。每个恒星群的参考光谱都是根据相对强度的量级范围（1% ∼ 99%）建立的。为了分离不同的恒星群，使用了五种不同的方法，如χ 2、余弦相似度、机器学习（ML）、等效宽度和线比。ML 和 χ 2 可以提供对某一恒星群的最佳和相对一致的预测。推导出的 RSG 星群下限能够达到红巨分支的 K s 波段顶端（K s ≈12.0 mag），表明其光度低至约 103.5 L ⊙，对应的恒星半径只有约 100 R ⊙。根据质量-光度关系 L / L ⊙ = f ( M / M ⊙ ) 3（f ≈ 15.5 ± 3），并考虑到迄今为止暗RSG的质量损失，RSG群体的最小初始质量约为6.1 ± 0.4 M ⊙，远低于传统的大质量恒星的临界值8 M ⊙。这是第一个光谱证据，表明RSG群体的质量下限约为6 M ⊙。然而，这类暗弱RSG的命运仍然难以捉摸，可能会对恒星演化和超新星模型产生巨大影响。
{"title":"Evolved Massive Stars at Low Metallicity. VII. The Lower Mass Limit of the Red Supergiant Population in the Large Magellanic Cloud","authors":"M. Yang 杨, Bo 博 Zhang 章, Biwei 碧沩 Jiang 姜, J. Gao 高, Y. Ren 任, Shu 舒 Wang 王, Man I 敏仪 Lam 林, H. Tian 田, Changqing 常青 Luo 罗, B. Chen 陈, Jing 静 Wen 文","doi":"10.3847/1538-4357/ad28c4","DOIUrl":"https://doi.org/10.3847/1538-4357/ad28c4","url":null,"abstract":"\u0000 The precise definition of the lower mass limit of red supergiant stars (RSGs) is an open question in astrophysics and does not attract much attention. Here, we assemble a spectroscopic evolved cool star sample with 6602 targets, including RSGs, asymptotic giant branch stars, and red giant branch stars, in the Large Magellanic Cloud based on Gaia DR3 and Sloan Digital Sky Survey IV/APOGEE-2. The reference spectrum of each stellar population is built according to the quantile range of relative intensity (1% ∼ 99%). Five different methods, e.g., χ\u0000 2, cosine similarity, machine learning (ML), equivalent width, and line ratio, are used in order to separate different stellar populations. ML and χ\u0000 2 provide the best and relatively consistent prediction of a certain population. The derived lower limit of the RSG population is able to reach the K\u0000 \u0000 s\u0000 -band tip of the red giant branch (K\u0000 \u0000 s\u0000 ≈12.0 mag), indicating a luminosity as low as about 103.5\u0000 L\u0000 ⊙, which corresponds to a stellar radius of only about 100 R\u0000 ⊙. Given the mass–luminosity relation of \u0000 \u0000\u0000\u0000 \u0000 L\u0000 \u0000 /\u0000 \u0000 \u0000 \u0000 L\u0000 \u0000 \u0000 ⊙\u0000 \u0000 \u0000 =\u0000 f\u0000 \u0000 \u0000 (\u0000 M\u0000 \u0000 /\u0000 \u0000 \u0000 \u0000 M\u0000 \u0000 \u0000 ⊙\u0000 \u0000 \u0000 )\u0000 \u0000 \u0000 3\u0000 \u0000 \u0000 \u0000 \u0000 with f ≈ 15.5 ± 3 and taking into account the mass loss of faint RSGs up to now, the minimal initial mass of the RSG population would be about 6.1 ± 0.4 M\u0000 ⊙, which is much lower than the traditional threshold of 8 M\u0000 ⊙ for the massive stars. This is the first spectroscopic evidence, indicating that the lower mass limit of the RSG population is around 6 M\u0000 ⊙. However, the destinies of such faint RSGs are still elusive and may have a large impact on stellar evolutionary and supernova models.","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"469 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140787995","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad2841
Runqing Jin, Meng Zhou, Y. Yi, H. Man, Z. Zhong, Y. Pang, Xiaohua Deng
Magnetic reconnection and turbulence are two of the most significant mechanisms for energy dissipation in collisionless plasma. The role of turbulence in magnetic reconnection poses an outstanding problem in astrophysics and plasma physics. It is still unclear whether turbulence can modify the reconnection process by enhancing the reconnection rate or energy conversion rate. In this study, utilizing unprecedented high-resolution data obtained from the Magnetospheric Multiscale spacecraft, we provide direct evidence that turbulence plays a vital role in promoting energy conversion during reconnection. We reached this conclusion by comparing magnetotail reconnection events with similar inflow Alfvén speed and plasma β but varying amplitudes of turbulence. The disparity in energy conversion was attributed to the strength of turbulence. Stronger turbulence generates more coherent structures with smaller spatial scales, which are pivotal contributors to energy conversion during reconnection. However, we find that turbulence has negligible impact on particle heating, but it does affect the ion bulk kinetic energy in these two events. These findings significantly advance our understanding of the relationship between turbulence and reconnection in astrophysical plasmas.
{"title":"Enhanced Energy Conversion by Turbulence in Collisionless Magnetic Reconnection","authors":"Runqing Jin, Meng Zhou, Y. Yi, H. Man, Z. Zhong, Y. Pang, Xiaohua Deng","doi":"10.3847/1538-4357/ad2841","DOIUrl":"https://doi.org/10.3847/1538-4357/ad2841","url":null,"abstract":"\u0000 Magnetic reconnection and turbulence are two of the most significant mechanisms for energy dissipation in collisionless plasma. The role of turbulence in magnetic reconnection poses an outstanding problem in astrophysics and plasma physics. It is still unclear whether turbulence can modify the reconnection process by enhancing the reconnection rate or energy conversion rate. In this study, utilizing unprecedented high-resolution data obtained from the Magnetospheric Multiscale spacecraft, we provide direct evidence that turbulence plays a vital role in promoting energy conversion during reconnection. We reached this conclusion by comparing magnetotail reconnection events with similar inflow Alfvén speed and plasma β but varying amplitudes of turbulence. The disparity in energy conversion was attributed to the strength of turbulence. Stronger turbulence generates more coherent structures with smaller spatial scales, which are pivotal contributors to energy conversion during reconnection. However, we find that turbulence has negligible impact on particle heating, but it does affect the ion bulk kinetic energy in these two events. These findings significantly advance our understanding of the relationship between turbulence and reconnection in astrophysical plasmas.","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"320 23","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140779788","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad3966
C. Esmerian, N. Gnedin
{"title":"Erratum: “Modeling Dust Production, Growth, and Destruction in Reionization-era Galaxies with the CROC Simulations: Methods and Parameter Exploration” (2022, ApJ, 940, 74)","authors":"C. Esmerian, N. Gnedin","doi":"10.3847/1538-4357/ad3966","DOIUrl":"https://doi.org/10.3847/1538-4357/ad3966","url":null,"abstract":"","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"366 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140776515","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad31ab
Ankita Ghosh, B. Bhattacharyya, A. Lyne, David L. Kaplan, J. Roy, P. Ray, B. Stappers, Sangita Kumari, Shubham Singh, Rahul Sharan
We present a timing solution for the 5.31 ms spider millisecond pulsar (MSP) J1242−4712, discovered with the GMRT. PSR J1242−4712 orbits a companion of minimum mass 0.08 M ⊙ with an orbital period of 7.7 hr and occupies a relatively unexplored region in the orbital period versus companion mass space. We did not detect gamma-ray pulsations for this MSP, and also could not identify the optical counterpart for PSR J1242–4712 in available optical/near-infrared data. The profile of J1242−4712 evolves with frequency, showing a clear single component at lower frequencies and a three-component profile at 650 MHz. PSR J1242−4712 eclipses for a very short duration near superior conjunction (orbital phase ∼ 0.23−0.25) below 360 MHz. Moreover, significant dispersion measure delays and errors in the pulse times of arrivals are observed near inferior conjunction (orbital phase ∼ 0.7), along with an observed eclipse in one epoch at 650 MHz. Observed eclipses and significant orbital period variability suggest that PSR J1242−4712 is possibly not a helium star−white dwarf binary, but has a semi- or nondegenerate companion, indicating that this is a “spider” MSP lying in a region between typical black widows and redbacks. This system may represent a distinct category of spider MSPs, displaying characteristics that bridge the gap between known black widow and redback MSPs.
{"title":"The GMRT High-resolution Southern Sky Survey for Pulsars and Transients. VII. Timing of the Spider Millisecond Pulsar PSR J1242–4712, a Bridge between Redback and Black Widow Pulsars","authors":"Ankita Ghosh, B. Bhattacharyya, A. Lyne, David L. Kaplan, J. Roy, P. Ray, B. Stappers, Sangita Kumari, Shubham Singh, Rahul Sharan","doi":"10.3847/1538-4357/ad31ab","DOIUrl":"https://doi.org/10.3847/1538-4357/ad31ab","url":null,"abstract":"\u0000 We present a timing solution for the 5.31 ms spider millisecond pulsar (MSP) J1242−4712, discovered with the GMRT. PSR J1242−4712 orbits a companion of minimum mass 0.08 M\u0000 ⊙ with an orbital period of 7.7 hr and occupies a relatively unexplored region in the orbital period versus companion mass space. We did not detect gamma-ray pulsations for this MSP, and also could not identify the optical counterpart for PSR J1242–4712 in available optical/near-infrared data. The profile of J1242−4712 evolves with frequency, showing a clear single component at lower frequencies and a three-component profile at 650 MHz. PSR J1242−4712 eclipses for a very short duration near superior conjunction (orbital phase ∼ 0.23−0.25) below 360 MHz. Moreover, significant dispersion measure delays and errors in the pulse times of arrivals are observed near inferior conjunction (orbital phase ∼ 0.7), along with an observed eclipse in one epoch at 650 MHz. Observed eclipses and significant orbital period variability suggest that PSR J1242−4712 is possibly not a helium star−white dwarf binary, but has a semi- or nondegenerate companion, indicating that this is a “spider” MSP lying in a region between typical black widows and redbacks. This system may represent a distinct category of spider MSPs, displaying characteristics that bridge the gap between known black widow and redback MSPs.","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"59 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140770295","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad2c8a
Tao Yan, Binzheng Zhang, Junjie Chen, Zhiqi Zheng, Ziyi Yang, Shengyi Ye, Jun Cui
Alfvénic power is generated through the interaction between the mini-magnetosphere of Ganymede and the corotating flow of the Jovian plasma, contributing to the formation of the Ganymede auroral footprint at Jupiter’s ionosphere. Using a three-dimensional, high-resolution global magnetohydrodynamic model of the Ganymede magnetosphere, we investigate the temporal variations of the Alfvénic power generated in the mini-magnetosphere of the moon under steady-state upstream conditions. Results show that (1) the Alfvénic power caused by the intermittent magnetic reconnections and the Kelvin–Helmholtz instabilities is quasiperiodic, varying over time with the periods about 71–333 s, which are consistent with the 100 s timescale periodicities of the Ganymede footprint's emitted power; and (2) the magnitude of the Alfvénic power is smaller when Ganymede is inside the Jovian plasma sheet where the B y component is smaller, and larger when the moon is outside the plasma sheet where the B y component is larger.
{"title":"Three-dimensional Magnetohydrodynamic Simulations of Periodic Variations of Ganymede’s Footprint","authors":"Tao Yan, Binzheng Zhang, Junjie Chen, Zhiqi Zheng, Ziyi Yang, Shengyi Ye, Jun Cui","doi":"10.3847/1538-4357/ad2c8a","DOIUrl":"https://doi.org/10.3847/1538-4357/ad2c8a","url":null,"abstract":"\u0000 Alfvénic power is generated through the interaction between the mini-magnetosphere of Ganymede and the corotating flow of the Jovian plasma, contributing to the formation of the Ganymede auroral footprint at Jupiter’s ionosphere. Using a three-dimensional, high-resolution global magnetohydrodynamic model of the Ganymede magnetosphere, we investigate the temporal variations of the Alfvénic power generated in the mini-magnetosphere of the moon under steady-state upstream conditions. Results show that (1) the Alfvénic power caused by the intermittent magnetic reconnections and the Kelvin–Helmholtz instabilities is quasiperiodic, varying over time with the periods about 71–333 s, which are consistent with the 100 s timescale periodicities of the Ganymede footprint's emitted power; and (2) the magnitude of the Alfvénic power is smaller when Ganymede is inside the Jovian plasma sheet where the B\u0000 \u0000 y\u0000 component is smaller, and larger when the moon is outside the plasma sheet where the B\u0000 \u0000 y\u0000 component is larger.","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"67 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140761235","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}
Pub Date : 2024-04-01DOI: 10.3847/1538-4357/ad3450
D. J. Yu
Observations reveal that surface and body modes exist in solar pores under photospheric conditions. While the effects of resonant absorption on photospheric surface modes are well established, its effect on body modes is not known yet. In this paper, we investigate resonant absorption for the body modes under photospheric conditions. We numerically solve the dispersion relation induced by thin boundary approximation and obtain the wave dispersion curves and damping rates of three arbitrarily chosen body modes for sausage and kink waves, respectively. The results show that resonant absorption for the body modes is weaker than for the slow surface modes in both cusp and Alfvén continua. The damping behavior of body modes is similar to slow surface modes while the higher body mode has stronger resonant absorption.
{"title":"Resonant Absorption of Magnetohydrodynamic Body Modes under Photospheric Conditions","authors":"D. J. Yu","doi":"10.3847/1538-4357/ad3450","DOIUrl":"https://doi.org/10.3847/1538-4357/ad3450","url":null,"abstract":"\u0000 Observations reveal that surface and body modes exist in solar pores under photospheric conditions. While the effects of resonant absorption on photospheric surface modes are well established, its effect on body modes is not known yet. In this paper, we investigate resonant absorption for the body modes under photospheric conditions. We numerically solve the dispersion relation induced by thin boundary approximation and obtain the wave dispersion curves and damping rates of three arbitrarily chosen body modes for sausage and kink waves, respectively. The results show that resonant absorption for the body modes is weaker than for the slow surface modes in both cusp and Alfvén continua. The damping behavior of body modes is similar to slow surface modes while the higher body mode has stronger resonant absorption.","PeriodicalId":504209,"journal":{"name":"The Astrophysical Journal","volume":"63 17","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140795120","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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