A systematic study of quiescent and outburst properties of X-ray-bright young stellar objects using XMM-Newton

@misc{sakuta2026systematic,
  title = {{A systematic study of quiescent and outburst properties of X-ray-bright young stellar objects using XMM-Newton}},
  author = {Koki Sakuta and Ikuyuki Mitsuishi and Seiya Sasamata and Daigo Nonaka and Mai Yamashita and Shin Toriumi and Takato Tokuno and Yohko Tsuboi and Hiroshi Kobayashi},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2607.25384},
  eprint = {2607.25384},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2607.25384},
}

TY  - UNPB
TI  - A systematic study of quiescent and outburst properties of X-ray-bright young stellar objects using XMM-Newton
AU  - Koki Sakuta
AU  - Ikuyuki Mitsuishi
AU  - Seiya Sasamata
AU  - Daigo Nonaka
AU  - Mai Yamashita
AU  - Shin Toriumi
AU  - Takato Tokuno
AU  - Yohko Tsuboi
AU  - Hiroshi Kobayashi
PY  - 2026
DA  - 2026/10/21
PB  - arXiv
DO  - 10.48550/arxiv.2607.25384
UR  - https://arxiv.org/abs/2607.25384
AB  - Young Stellar Objects (YSOs) exhibit strong X-ray emission, widely attributed to magnetic reconnection and magnetospheric accretion; however, owing primarily to limited photon statistics, observational tests of these mechanisms have often relied on simplified analyses, leaving room for more precise constraints on their emission processes. We aim to derive the X-ray properties of X-ray-bright YSOs selected from multiple star clusters and investigate their emission mechanisms through an approach from multiple perspectives based on timing and spectroscopic analysis. We performed a systematic search of XMM-Newton archival observations and constructed a sample of 51 X-ray-bright YSOs for timing and spectroscopic analyses. We identified quiescent and outburst phases through timing analysis, performed phase-resolved multi-temperature spectroscopy. Multi-temperature plasma structures are detected in both quiescent and outburst emission. The relationships among the timing and spectral parameters are broadly consistent with a magnetic-reconnection scenario. Comparison with Gaia DR3 stellar parameters suggests that magnetospheric accretion alone has difficulty explaining most of the fitted X-ray temperatures, although the coolest model components with kT ≲ 0.3 keV may include an accretion-shock contribution. After separating these low-temperature components, the remaining quiescent components show a clearer positive correlation in the EM--kT plane, with magnetic-loop lengths distributed around 10^12 cm. Neupert-like behavior, the temporal evolution of temperature and emission measure, the Rossby-number activity relation, and positive correlations between quiescent and outburst properties all suggest that magnetic reconnection plays a key role in both phases.
ER  -