학술논문
The High Energy X-ray Probe (HEX-P): Galactic PeVatrons, star clusters, superbubbles, microquasar jets, and gamma-ray binaries
Document Type
Working Paper
Author
Mori, Kaya; Reynolds, Stephen; An, Hongjun; Bamba, Aya; Krivonos, Roman; Tsuji, Naomi; Abdelmaguid, Moaz; Alford, Jason; Bangale, Priyadarshini; Celli, Silvia; Diesing, Rebecca; Eagle, Jordan; Fryer, Chris L.; Gabici, Stefano; Gelfand, Joseph; Grefenstette, Brian; Garcia, Javier; Kim, Chanho; Kumar, Sajan; Kuznetsova, Ekaterina; Mac Intyre, Brydyn; Madsen, Kristin; Manconi, Silvia; Motogami, Yugo; Ohsumi, Hayato; Olmi, Barbara; Park, Jaegeun; Ponti, Gabriele; Sato, Toshiki; Shang, Ruo-Yu; Stern, Daniel; Terada, Yukikatsu; Woo, Jooyun; Younes, George; Zoglauer, Andreas
Source
Subject
Language
Abstract
HEX-P is a probe-class mission concept that will combine high spatial resolution X-ray imaging (<10" FWHM) and broad spectral coverage (0.2-80 keV) with an effective area far superior to current facilities (including XMM-Newton and NuSTAR) to enable revolutionary new insights into a variety of important astrophysical problems. With the recent discoveries of over 40 ultra-high-energy gamma-ray sources (detected above 100 TeV) and neutrino emission in the Galactic Plane, we have entered a new era of multi-messenger astrophysics facing the exciting reality of Galactic PeVatrons. In the next decade, as more Galactic PeVatrons and TeV gamma-ray sources are expected to be discovered, the identification of their acceleration and emission mechanisms will be the most pressing issue in both particle and high-energy astrophysics. In this paper, along with its companion papers (Reynolds et al. 2023, Mori et al. 2023), we will present that HEX-P is uniquely suited to address important problems in various cosmic-ray accelerators, including Galactic PeVatrons, through investigating synchrotron X-ray emission of TeV-PeV electrons produced by both leptonic and hadronic processes.
Comment: 31 pages, 12 figures, submitted to FrASS
Comment: 31 pages, 12 figures, submitted to FrASS