两颗发射X射线的Be星的多波段综合研究
A comprehensive multi-wavelength study of two X-ray emitting Be stars
- CHRIST (Deemed to be University)（克里斯特（视为大学））
- The Centre of Excellence in Astronomy and Astrophysics (CEAA), CHRIST (Deemed to be University)（天文学与天体物理学卓越中心，克里斯特（视为大学））
- St. Francis de Sales College (Autonomous)（圣方济各沙雷氏学院（自治））
- INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所 - 阿切特里天文台）
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AI总结：
本研究对两颗Be星进行多波段分析，确定其一为经典Be星、另一为吸积型Herbig Be星，并发现其X射线发射源于磁影响的星周活动，支持磁约束风激波或磁力矩盘模型。
AI中文摘要：
我们展示了对两颗发射X射线的Be星——CXOU J052218.4+332820（恒星1）和CXOU J052304.2+332846（恒星2）——的多波段研究，这两颗恒星是从LAMOST DR5热发射线恒星目录中识别出来的。我们的光谱和光度分析表明，恒星1是一颗主序B5e星，而恒星2是一颗前主序B7e星。恒星1的LAMOST光谱显示出来自星周区域的壳层型Feii、帕申系和Oi发射，该区域延伸至约3-5Rstar。TESS周期分析揭示了一个约0.355天的快速自转周期和约68度的倾角，证实了恒星1的经典Be星性质。相比之下，恒星2显示出强烈的吸积特征，包括逆P-Cygni Feii和红移的Hei吸收特征。其ZTF光变曲线显示出高达约3星等的非规则变暗事件以及约50-110天时间尺度上的准周期变化，与吸积型Herbig Be星中的星周消光现象一致。为了进一步研究这两个系统的高能特性，我们分析了它们的Chandra X射线光谱。Chandra光谱学得出中等等离子体温度（kT约1.7-1.8 keV）和X射线光度logL_X约30.4-30.6 erg/s，与磁活动冕中观测到的值相当。此外，Chandra和Gaia坐标之间的位置一致性表明，X射线发射在空间上与光学系统相关联，而非附近已分辨的伴星。这些结果表明，观测到的X射线发射源于受磁影响的星周活动，与磁约束风激波（MCWS）或磁力矩盘情景一致。
英文摘要：
We present a multi-wavelength study of two X-ray-emitting Be stars, CXOU J052218.4+332820 (Star 1) and CXOU J052304.2+332846 (Star 2), identified from the LAMOST DR5 Hot emission-line stars catalog. Our spectroscopic and photometric analyses indicate that Star 1 is a main-sequence B5e star, whereas Star 2 is a pre-main-sequence B7e star. The LAMOST spectrum of Star 1 exhibits shell-type Feii, Paschen, and Oi emission from circumstellar regions extending to ~ 3 - 5Rstar. TESS period analysis reveals a rapid rotational period of ~ 0.355 d and an inclination angle of ~ 68 deg, confirming the Classical Be nature of Star 1. In contrast, Star 2 shows strong accretion signatures, including inverse P-Cygni Feii and redshifted Hei absorption features. Its ZTF light curves display irregular dimming events of up to ~ 3 mag and quasi-periodic variability on timescales of ~ 50 - 110 d, consistent with circumstellar obscuration in an accreting Herbig Be star. To further investigate the high-energy properties of the two systems, we analyzed their Chandra X-ray spectra. Chandra spectroscopy yields moderate plasma temperatures (kT ~ 1.7-1.8 keV) and X-ray luminosities of logL_X ~ 30.4-30.6 erg/s, comparable to those observed in magnetically active coronae. Furthermore, the positional agreement between the Chandra and Gaia coordinates indicates that the X-ray emission is spatially associated with the optical systems rather than a nearby resolved companion. These results suggest that the observed X-ray emission originates from magnetically influenced circumstellar activity, consistent with magnetically confined wind-shock (MCWS) or magnetically torqued disk scenarios.
