Search for High-Energy Neutrinos from Infrared Flares
Loyola University Chicago(洛约拉大学芝加哥分校);Deutsches Elektronen-Synchrotron DESY(德国电子同步加速器);University of Canterbury(坎特伯雷大学);Université Libre de Bruxelles(布鲁塞尔自由大学);Niels Bohr Institute, University of Copenhagen(哥本哈根大学尼尔斯玻尔研究所);TU Dortmund University(多特蒙德工业大学);University of Kansas(堪萨斯大学);Bartol Research Institute and Dept. of Physics and Astronomy, University of Delaware(特拉华大学巴托尔研究所及物理与天文学系);Marquette University(马凯特大学);Harvard University(哈佛大学);Michigan State University(密歇根州立大学);South Dakota School of Mines and Technology(南达科他矿业理工学院)
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, J. M. Alameddine, S. Ali, N. M. Amin, K. Andeen, C. Arg{ü}elles, S. Athanasiadou, S. N. Axani, R. B… 展开作者
R. Abbasi, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, J. M. Alameddine, S. Ali, N. M. Amin, K. Andeen, C. Arg{ü}elles, S. Athanasiadou, S. N. Axani, R. Babu, X. Bai, A. Balagopal V., S. W. Barwick, V. Basu, R. Bay, J. J. Beatty, J. Becker Tjus, J. Beise, C. Bellenghi, S. Benkel, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, E. Blaufuss, L. Bloom, S. Blot, F. Bontempo, J. Y. Book Motzkin, C. Boscolo Meneguolo, S. B{ö}ser, O. Botner, J. Braun, B. Brinson, Z. Brisson-Tsavoussis, L. Brusa, R. T. Burley, D. Butterfield, K. Carloni, J. Carpio, N. Chau, Y. C. Chen, Z. Chen, D. Chirkin, S. Choi, A. Chubarov, B. A. Clark, D. A. Coloma Borja, A. Connolly, J. M. Conrad, D. F. Cowen, C. De Clercq, J. J. DeLaunay, D. Delgado, T. Delmeulle, S. Deng, P. Desiati, K. D. de Vries, G. de Wasseige, T. DeYoung, J. C. D{\'ı}az-V{é}lez, S. DiKerby, T. Ding, M. Dittmer, A. Domi, L. Draper, L. Dueser, D. Durnford, K. Dutta, M. A. DuVernois, T. Ehrhardt, L. Eidenschink, A. Eimer, C. Eldridge, P. Eller, E. Ellinger, D. Els{ä}sser, R. Engel, H. Erpenbeck, W. Esmail, S. Eulig, J. Evans, P. A. Evenson, K. L. Fan, K. Fang, K. Farrag, A. Fattorini, A. R. Fazely, A. Fedynitch, N. Feigl, C. Finley, D. Fox, A. Franckowiak, S. Fukami, P. F{ü}rst, J. Gallagher, A. Garcia, M. Garcia, E. Genton, L. Gerhardt, A. Ghadimi, C. Glaser, T. Gl{ü}senkamp, J. G. Gonzalez, S. Goswami, A. Granados, D. Grant, S. J. Gray, S. Griffin, S. Griswold, K. M. Groth, D. Guevel, C. G{ü}nther, P. Gutjahr, C. Ha, A. Hallgren, F. Halzen, M. Handt, K. Hanson, J. Hardin, A. A. Harnisch, P. Hatch, A. Haungs, J. H{ä}ußler, K. Helbing, J. Hellrung, B. Henke, L. Hennig, F. Henningsen, L. Heuermann, R. Hewett, N. Heyer, S. Hickford, A. Hidvegi, C. Hill, G. C. Hill, R. Hmaid, K. D. Hoffman, A. Hollnagel, D. Hooper, S. Hori, K. Hoshina, M. Hostert, W. Hou, M. Hrywniak, T. Huber, K. Hultqvist, K. Hymon, A. Ishihara, W. Iwakiri, M. Jacquart, S. Jain, O. Janik, M. Jansson, M. Jin, N. Kamp, D. Kang, W. Kang, A. Kappes, L. Kardum, T. Karg, A. Karle, A. Katil, M. Kauer, J. L. Kelley, B. Kern, M. Khanal, A. Khatee Zathul, A. Kheirandish, T. Kim, H. Kimku, F. Kirchner, J. Kiryluk, C. Klein, S. R. Klein, Y. Kobayashi, S. Koch, A. Kochocki, R. Koirala, H. Kolanoski, T. Kontrimas, L. K{ö}pke, C. Kopper, D. J. Koskinen, P. Koundal, M. Kowalski, A. Kravka, N. Krieger, T. Krishnan, K. Kruiswijk, E. Krupczak, E. Kun, N. Kurahashi, C. Lagunas Gualda, L. Lallement Arnaud, M. J. Larson, F. Lauber, J. P. Lazar, K. Leonard DeHolton, A. Leszczy{ń}ska, C. Li, J. Liao, C. Lin, Q. R. Liu, Y. T. Liu, M. Liubarska, C. Love, L. Lu, F. Lucarelli, W. Luszczak, Y. Lyu, M. Macdonald, F. Machingal, E. Magnus, Y. Makino, E. Manao, S. Mancina, A. Mand, I. C. Mari{ş}, S. Marka, Z. Marka, I. Martinez-Soler, R. Maruyama, J. Mauro, F. Mayhew, F. McNally, K. Meagher, A. Medina, M. Meier, Y. Merckx, L. Merten, J. M. Mitchell, S. Mondal, T. Montaruli, R. W. Moore, Y. Morii, A. Mosbrugger, D. Mousadi, E. Moyaux, T. Mukherjee, M. Nakos, U. Naumann, R. Neshat, L. Neste, M. Neumann, M. U. Nisa, K. Noda, A. Noell, A. Novikov, A. Obertacke, V. O'Dell, A. Olivas, R. Orsoe, J. Osborn, E. O'Sullivan, B. Owens, V. Palusova, H. Pandya, A. Parenti, C. Parisel, N. Park, V. Parrish, E. N. Paudel, L. Paul, C. P{é}rez de los Heros, T. Pernice, T. C. Petersen, J. Peterson, S. Pick, M. Plum, A. Pont{é}n, V. Poojyam, B. Pries, R. Procter-Murphy, G. T. Przybylski, L. Pyras, C. Raab, J. Rack-Helleis, N. Rad, M. Ravn, K. Rawlins, Z. Rechav, A. Rehman, R. Reimann, I. Reistroffer, E. Resconi, C. D. Rho, W. Rhode, L. Ricca, B. Riedel, A. Rifaie, E. J. Roberts, S. Rodan, M. Rongen, A. Rosted, C. Rott, T. Ruhe, L. Ruohan, D. Ryckbosch, J. Saffer, D. Salazar-Gallegos, P. Sampathkumar, A. Sandrock, G. Sanger-Johnson, M. Santander, S. Sarkar, M. Scarnera, M. Schaufel, H. Schieler, S. Schindler, L. Schlickmann, B. Schl{ü}ter, F. Schl{ü}ter, N. Schmeisser, T. Schmidt, F. Schmitt, A. Scholz, F. G. Schr{ö}der, S. Schwirn, S. Sclafani, D. Seckel, L. Seen, M. Seikh, S. Seunarine, P. A. Sevle Myhr, R. Shah, S. Shah, A. Sharma, S. Shefali, N. Shimizu, M. Shin, R. Singh, B. Skrzypek, R. Snihur, J. Soedingrekso, D. Soldin, P. Soldin, G. Sommani, D. Song, C. Spannfellner, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, T. Stezelberger, T. St{ü}rwald, T. Stuttard, G. W. Sullivan, I. Taboada, S. Ter-Antonyan, A. Terliuk, A. Thakuri, P. Thelen, M. Thiesmeyer, W. G. Thompson, J. Thwaites, W. Tian, S. Tilav, K. Tollefson, J. A. Torres, S. Toscano, D. Tosi, K. Upshaw, A. Vaidyanathan, N. Valtonen-Mattila, J. Valverde, J. Vandenbroucke, T. Van Eeden, N. van Eijndhoven, L. Van Rootselaar, J. van Santen, J. Vara, F. Varsi, M. Velazquez, M. Venugopal, M. Vereecken, S. Vergara Carrasco, S. Verpoest, A. Vijai, J. Villarreal, C. Walck, A. Wang, E. H. S. Warrick, C. Weaver, P. Weigel, A. Weindl, J. Weldert, A. Y. Wen, C. Wendt, J. Werthebach, M. Weyrauch, N. Whitehorn, C. H. Wiebusch, D. R. Williams, L. Witthaus, J. Woodward, G. Wrede, X. W. Xu, J. P. Yanez, Y. Yao, E. Yildizci, S. Yoshida, F. Yu, S. Yu, T. Yuan, S. Yun-C{á}rcamo, A. Zander Jurowitzki, A. Zegarelli, S. Zhang, Z. Zhang, P. Zhelnin, P. Zilberman, C. Zilleruelo Ca{ñ}as, M. Zimmermann
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10 pages, 3 figures, To be submitted to Astronomy & Astrophysics
IceCube has detected a diffuse flux of high-energy astrophysical neutrinos. While its astrophysical origin is unknown, a significant neutrino emission has been observed from the gamma-ray blazar TXS 0506+056 and the Seyfert galaxy NGC 1068. This suggests accretion by supermassive black holes as one of the candidate mechanisms of the diffuse neutrino flux. Indeed, external studies that made use of IceCube data identified candidate sources, including AT2019dsg, likely a stellar tidal disruption event (TDE), and AT2019fdr, associated with an active galactic nucleus (AGN). An additional study using an optically detected sample of 63 accretion flares revealed another candidate as a potential high-energy neutrino counterpart: AT2019aalc. All of these candidate transients exhibit strong dust echoes, characterized by delayed infrared (IR) emission relative to the initial optical outburst. We look for correlations between the most comprehensive catalog of infrared flares and 10 years of IceCube archival data. We perform a time-dependent stacking analysis testing 393 sources in the Northern Sky against 10 years of through-going tracks. No significant neutrino emission is observed, and we derive upper limits to constrain neutrino emission from this catalog. These limits are subsequently extrapolated to a population-level study. We find that the contribution of IR flares to the IceCube diffuse neutrino flux at 100 TeV is below 2.7% for a spectral index of 2.5.
High-energy neutrinos from X-rays flares of blazars frequently observed by the Swift X-Ray Telescope
Blazar耀斑被认为是增强中微子产生的理想候选者。虽然$γ$射线耀斑的中微子信号已被广泛讨论,但X射线耀斑的中微子产额却很少受到关注。在这里,我们计算预测的中微子信号从X射线耀斑检测到66耀变体观测超过50倍的X射线望远镜(XRT)上的尼尔Gehrels斯威夫特天文台。我们考虑的情况下,X射线耀斑是由相对论质子的同步辐射,中微子是通过质子与它们自己的同步X射线光子之间的光子相互作用产生的。利用1 keV的X射线光变曲线进行耀斑鉴别,用0.5-10 keV的耀斑能量密度作为全味中微子能量密度的代用品,以及不同探测器配置下IceCube点源的有效面积,计算了IceCube在每个耀斑源上产生的100 TeV以上的μ子和反μ子中微子的数量。样品中的大部分中微子事件来自持续时间为$\sim 1-10$ d的耀斑。考虑到样本中源的X射线耀斑占空比(范围在$\sim2$和24%之间),我们计算出每个源的平均年中微子率。分布中位数(对数)为$\sim0.03$ yr $^{-1}$,Mkn 421的$1.2\pm 0.3$ yr $^{-1}$预测率最高,其次是3C 273 $(0.33\pm0.03$ yr $^{-1})$和PG 1553+113($0.25\pm0.02$ yr $^{-1}$)。下一代中微子探测器与对耀变体的定期X射线监测一起可以限制强子X射线耀斑的占空比。
Testing the Association of Supermassive Black Hole Infrared Flares and High-energy Neutrinos
MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology(麻省理工学院);Department of Astronomy and Columbia Astrophysics Laboratory, Columbia University(哥伦比亚大学);Center for Computational Astrophysics, Flatiron Institute(西蒙斯基金会平顿研究所计算天体物理中心);Department of Physics, Norwegian University of Science and Technology(挪威科技大学)
A magnetohydrodynamic model for multi-wavelength flares from Sagittarius~A$^\star$ (I): model and the near-infrared and X-ray flares
我们银河系中的超大质量黑洞人马座~A $^\star$(Sgr A $^\star$)的耀斑在过去十年左右被定期观测到。尽管有许多观测和理论上的努力,这种耀斑的性质仍然知之甚少,虽然一些现象学的方案已经提出。在这项工作中,我们将Yuan等人(2009)的方案发展为Sgr A $^\star$耀斑的磁流体动力学(MHD)模型。该模型与太阳物理学中太阳耀斑和日冕物质抛射理论类似。在该模型中,磁场环出现从吸积流到Sgr A $^\star$和扭曲,形成磁通绳,因为剪切和湍流。在这个过程中,磁能也被积累,直到达到阈值。然后,在电流片中的磁重联的帮助下,这导致通量绳的灾难性演变。在这个灾难性的过程中,磁能被部分转换为非热电子的能量。定量计算了耀斑区磁绳的高度、大小、速度、磁场的动力学演化以及相对论电子的能量分布。我们进一步计算了这些电子的同步辐射,并将得到的光变曲线与观测值进行了比较。结果表明,该模型能够合理地解释近红外和X射线耀斑的主要观测结果,包括它们的光变曲线和光谱。它也可以解释射电耀斑光变曲线中频率依赖的时间延迟。
Could a plasma in quasi-thermal equilibrium be associated to the "orphan" TeV flares ?
TeV $γ$ -射线探测在耀斑状态下没有活动的X射线从耀变体吸引了很多关注,由于这些“孤儿”耀斑的不规则性。虽然同步加速器自康普顿模型已经非常成功地解释了这些源的光谱能量分布和光谱可变性,它还没有能够描述这些非典型的耀斑事件。另一方面,在AGN喷流底部的电子-正电子对等离子体被认为是相对论外流体加速的机制。这种处于准热平衡的等离子体被称为温火球,它发射出MeV峰值能量的辐射,作为加速质子的目标。在这项工作中,我们描述了“孤儿”TeV耀斑耀变体1 ES 1959+650和Mrk 421假设几何考虑在射流和引起费米加速质子和MeV峰值目标光子来自温火球的相互作用。在成功地描述了这些“孤儿”TeV耀斑后,我们关联了TeV $γ$射线、中微子和UHECR通过p $γ$相互作用的通量,并分别计算了IceCube/AMANDA和TA实验中预期的高能中微子和UHECR的数目.此外,在Wein火球中主要通过电子正电子湮没产生的MeV热中微子也可以通过它传播.通过考虑两个中微子(太阳、大气和加速器参数)和三个中微子的混合,我们研究了共振振荡,估计了中微子味比以及地球上预期的热中微子数量.
Upstream neutrino production and delayed jet emission in the blazar GB6 J1542+6129
ELTE(匈牙利罗兰大学);Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences(孔科利天文台,HUN-REN 天文学与地球科学研究中心);CSFK, MTA Centre of Excellence(CSFK,MTA 卓越中心);Ruhr University Bochum(波鸿鲁尔大学);University of Florida(佛罗里达大学);University of Szeged(塞格德大学);Chalmers University of Technology(查尔姆斯理工大学);Max Planck Institute for Radio Astronomy(马克斯·普朗克射电天文研究所);University of Alabama(阿拉巴马大学)
A neutrino flare candidate potentially associated with X-ray emission from tidal disruption event ATLAS17jrp
Purple Mountain Observatory, Chinese Academy of Sciences(中国科学院紫金山天文台);University of Science and Technology of China(中国科学技术大学);Deutsches Elektronen-Synchrotron DESY(德国电子同步加速器)
研究发现一个可能与 tidal disruption 事件 ATLAS17jrp 发射的 X 射线相关的中微子喷流候选者,通过质子-光子过程产生中微子。