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SUMMARY:Unveiling Multimessenger Emission from Hidden Cores of Microquasar
 s
DTSTART;VALUE=DATE-TIME:20260522T053000Z
DTEND;VALUE=DATE-TIME:20260522T063000Z
DTSTAMP;VALUE=DATE-TIME:20260522T102700Z
UID:indico-event-5038@indico-tdli.sjtu.edu.cn
DESCRIPTION:Speakers: Yu-Jia Wei (Pennsylvania State University)\n\nAbstra
 ct: Microquasars are radio-emitting X-ray binaries accompanied by relativ
 istic jets. They are established sources of 100~TeV gamma rays and are con
 sidered promising candidates for cosmic-ray acceleration.Motivated by rece
 nt detections of $\\sim 100~$TeV photons from Cygnus~X-1 and multi-PeV pho
 tons from Cygnus~X-3 by the Large High Altitude Air Shower Observatory (LH
 AASO)\, we employ the Astrophysical Multimessenger Emission Simulator (AME
 S) to model their multimessenger emission considering compact outflow regi
 ons as cosmic-ray accelerators\, spanning from radio to ultrahigh-energy g
 amma rays. Our results show that the observed $>$TeV gamma rays can origin
 ate from either $p\\gamma$ or $pp$ interactions\, depending on the locatio
 n and physical conditions of the emission region\, while also reproducing 
 the lower-energy spectra. These different configurations of emission regio
 ns yield unique\, observationally testable predictions. In the $0.1-10$~Te
 V energy range\, where current observations provide only upper limits\, th
 e models predict either a deep dip\, a mild suppression\, or a power-law s
 pectrum. Additionally\, models involving compact emission regions comparab
 le to the orbital separation predict strong variability\, while those invo
 king more extended and static external zones show more stable behavior. We
  also provide a possible qualitative explanation for the distinct modulati
 on patterns across different energy bands\, which relies primarily on chan
 ges in the Doppler factor and external $\\gamma\\gamma$ absorption. In par
 ticular\, as a result\, we find that explaining the PeV emission from Cygn
 us~X-3 favors a compact emission region\, for which a magnetic field stren
 gth of order $\\sim 10^2~\\mathrm{G}$ is required. Finally\, our neutrino 
 predictions\, which properly account for muon and pion cooling effects\, r
 eveal a significantly suppressed flux\, indicating that detecting these so
 urces may be more challenging than previously anticipated.Presentation of 
 the presenter:  Yu-Jia Wei is a Ph.D. student in the Department of Astro
 nomy and Astrophysics at the Pennsylvania State University. Before joining
  Penn State\, she received her M.S. from Purple Mountain Observatory\, and
  her B.S. from Nanjing University. Her theoretical work focuses on high-en
 ergy astrophysics and multimessenger astronomy\, with a particular interes
 t in jet-related sources and gravitational-wave progenitors\, such as gamm
 a-ray bursts\, fast radio bursts\, X-ray binaries\, and blazars.Alternativ
 e online link: https://meeting.tencent.com/dm/7c5T4Cm1O1wJ ID: 574530481
 \n\nhttps://indico-tdli.sjtu.edu.cn/event/5038/
LOCATION:Tsung-Dao Lee Institute/N6F-N600 - Lecture Room (Tsung-Dao Lee In
 stitute)
URL:https://indico-tdli.sjtu.edu.cn/event/5038/
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