Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Articles Article Faculty Publications -Articles Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Chandra X-ray analysis of Herbig Ae/Be stars Subject The topic of the resource stars: coronae; stars: flare; stars: low-mass; stars: massive; stars: pre-main-sequence; techniques: imaging spectroscopy Description An account of the resource Herbig Ae/Be (HAeBe) stars are intermediate-mass pre-main-sequence stars, characterized by infrared (IR) excess and emission lines. They are observed to emit X-rays, whose origin is a matter of discussion and not settled yet. X-ray emission is not expected in HAeBe stars, as they lack the subsurface convective zone. In this study, we retrieved observations from the Chandra archive for 62 HAeBe stars, among which 44 sources (detection fraction ?71 per cent) were detected in X-rays, with 7 being new detections. We use this sample as a test bed to conduct a comparative analysis of the X-ray properties of HAeBe stars and their low-mass counterparts, T Tauri stars (TTSs). Further, we compare the X-ray properties of HAeBe stars and TTSs with optical and IR properties to constrain the X-ray emission mechanism in HAeBe stars. We found no correlation between X-ray emission and disc properties of HAeBe stars, confirming that X-rays are not related to accretion shocks. About 56 per cent of HAeBe stars without any known subarcsec companions have lower plasma temperatures (kT ? 2 keV). We observe flaring/variability in HAeBe stars with confirmed low-mass companions. These stars show plasma temperatures &gt; 2 keV, similar to TTSs. Guided by this information, we discuss the role of a T Tauri companion for X-ray emission seen in our sample of HAeBe stars. From the results obtained in this paper, we suggest that X-ray emission from HAeBe stars may not be related to accretion shocks or hidden TTS, but rather can be due to magnetically driven coronal emission. 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. Creator An entity primarily responsible for making the resource Anilkumar H.; Mathew B.; Jithesh V.; Kartha S.S.; Manoj P.; Narang M.; Chavali M. Source A related resource from which the described resource is derived Monthly Notices of the Royal Astronomical Society, Vol-530, No. 3, pp. 3020-3037. Publisher An entity responsible for making the resource available Oxford University Press Date A point or period of time associated with an event in the lifecycle of the resource 2024-01-01 Identifier An unambiguous reference to the resource within a given context <a href="https://doi.org/10.1093/mnras/stae938" target="_blank" rel="noreferrer noopener">https://doi.org/10.1093/mnras/stae938</a> <br /><br /><a href="https://www.scopus.com/inward/record.uri?eid=2-s2.0-85193382959&amp;doi=10.1093%2Fmnras%2Fstae938&amp;partnerID=40&amp;md5=f08a0ccd443a60016e5d6433d684d703" target="_blank" rel="noreferrer noopener">https://www.scopus.com/inward/record.uri?eid=2-s2.0-85193382959&amp;doi=10.1093%2fmnras%2fstae938&amp;partnerID=40&amp;md5=f08a0ccd443a60016e5d6433d684d703</a> Rights Information about rights held in and over the resource All Open Access; Gold Open Access Relation A related resource ISSN: 358711; CODEN: MNRAA Format The file format, physical medium, or dimensions of the resource Online Language A language of the resource English Type The nature or genre of the resource Article Coverage The spatial or temporal topic of the resource, the spatial applicability of the resource, or the jurisdiction under which the resource is relevant Anilkumar H., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore, 560029, India; Mathew B., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore, 560029, India; Jithesh V., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore, 560029, India; Kartha S.S., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore, 560029, India; Manoj P., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai, 400005, India; Narang M., Academia Sinica Institute of Astronomy and Astrophysics, 11F of Astro-Math Bldg., No. 1, Section 4, Roosevelt Road Republic of China, Taipei, 10617, Taiwan; Chavali M., Max Planck Institute for Radio Astronomy, Auf dem Hel 69, Bonn, D-53121, Germany