A Multiwavelength View of $ρ$ Oph I: Resolving the X-ray Source Between A and B
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| Main Authors: | , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866908568878317568 |
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| author | Gunderson, Sean J. Codd, Jackson Golay, Walter W. Huenemoerder, David P. Cannon, John M. Fluegel, J. Alex Griffin, Philip E. Haurberg, Nathalie C. Ignace, Richard Moreno, Alexandrea Pradhan, Pragati Riggs, Alexis Wetzel, James Canizares, Claude R. consortium, the MACRO |
| author_facet | Gunderson, Sean J. Codd, Jackson Golay, Walter W. Huenemoerder, David P. Cannon, John M. Fluegel, J. Alex Griffin, Philip E. Haurberg, Nathalie C. Ignace, Richard Moreno, Alexandrea Pradhan, Pragati Riggs, Alexis Wetzel, James Canizares, Claude R. consortium, the MACRO |
| contents | We present a multiwavelength analysis of the central stellar pair of $ρ$ Oph, components A and B. Using recent high-resolution \textit{Chandra X-ray Observatory} observations, we demonstrate with high confidence that the dominant X-ray source is $ρ$ Oph B, while $ρ$ Oph A is comparatively X-ray faint. This result contrasts with earlier \textit{XMM-Newton} observations, which, due to limited spatial resolutions, attributed the X-ray emission to $ρ$ Oph A. An analysis of $ρ$ Oph B's X-ray light curves and spectra reveals properties more consistent with a cool star than a hot star. We therefore propose that $ρ$ Oph B is an Algol-like binary system, consisting of a B-type primary and an active, X-ray-emitting GK-type companion. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_26268 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A Multiwavelength View of $ρ$ Oph I: Resolving the X-ray Source Between A and B Gunderson, Sean J. Codd, Jackson Golay, Walter W. Huenemoerder, David P. Cannon, John M. Fluegel, J. Alex Griffin, Philip E. Haurberg, Nathalie C. Ignace, Richard Moreno, Alexandrea Pradhan, Pragati Riggs, Alexis Wetzel, James Canizares, Claude R. consortium, the MACRO Solar and Stellar Astrophysics High Energy Astrophysical Phenomena We present a multiwavelength analysis of the central stellar pair of $ρ$ Oph, components A and B. Using recent high-resolution \textit{Chandra X-ray Observatory} observations, we demonstrate with high confidence that the dominant X-ray source is $ρ$ Oph B, while $ρ$ Oph A is comparatively X-ray faint. This result contrasts with earlier \textit{XMM-Newton} observations, which, due to limited spatial resolutions, attributed the X-ray emission to $ρ$ Oph A. An analysis of $ρ$ Oph B's X-ray light curves and spectra reveals properties more consistent with a cool star than a hot star. We therefore propose that $ρ$ Oph B is an Algol-like binary system, consisting of a B-type primary and an active, X-ray-emitting GK-type companion. |
| title | A Multiwavelength View of $ρ$ Oph I: Resolving the X-ray Source Between A and B |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2509.26268 |