The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II Disk
Variability of millimeter wavelength continuum emission from Class II protoplanetary disks is extremely rare, and when detected, it is usually interpreted as originating from nonthermal emission mechanisms that relate to the host star itself rather than its disk. During observations made as part of...
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2025-01-01
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| author | James M. Miley Laura M. Pérez Carolina Agurto-Gangas Anibal Sierra Leon Trapman Miguel Vioque Nicolas Kurtovic Paola Pinilla Ilaria Pascucci Ke Zhang Rossella Anania John Carpenter Lucas A. Cieza Dingshan Deng Camilo González-Ruilova Giovanni P. Rosotti Dary A. Ruiz-Rodriguez Estephani E. TorresVillanueva |
| author_facet | James M. Miley Laura M. Pérez Carolina Agurto-Gangas Anibal Sierra Leon Trapman Miguel Vioque Nicolas Kurtovic Paola Pinilla Ilaria Pascucci Ke Zhang Rossella Anania John Carpenter Lucas A. Cieza Dingshan Deng Camilo González-Ruilova Giovanni P. Rosotti Dary A. Ruiz-Rodriguez Estephani E. TorresVillanueva |
| author_sort | James M. Miley |
| collection | DOAJ |
| description | Variability of millimeter wavelength continuum emission from Class II protoplanetary disks is extremely rare, and when detected, it is usually interpreted as originating from nonthermal emission mechanisms that relate to the host star itself rather than its disk. During observations made as part of the AGE-PRO Large Program, significant variability in the brightness of the 2MASS J16202863-2442087 system was detected between individual executions. We report the observed properties of the variability detected at millimeter wavelengths and investigate potential driving mechanisms. To investigate the nature of the variability, we construct a light curve from the continuum observations and analyze images constructed from both flaring and quiescent emission. We characterize the dust disk around the star through analysis in the image and visibility plane, and carry out kinematic analysis of CO (2–1) emission from the gas disk. The continuum flux decays by a factor of 8 in less than an hour, and by a factor of 13 within 8 days. The peak brightness coincides with an expected brightness maximum extrapolated from the periodicity of previously observed optical variability. The flare is most likely the product of synchrotron emission in the close vicinity of the star. The nature of the millimeter flare closely resembles those detected in very close binary systems, and may be due to the interaction of magnetic fields in an as-yet undetected binary. Alternatively, if the central host is a single-star object, the flare may be due to the interaction of magnetic field loops at the stellar surface or a strong accretion burst. |
| format | Article |
| id | doaj-art-8b2e4e1379314e35b96b86cd3b19bb4c |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-8b2e4e1379314e35b96b86cd3b19bb4c2025-08-20T03:39:19ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198911110.3847/1538-4357/add25cThe ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II DiskJames M. Miley0https://orcid.org/0000-0002-1575-680XLaura M. Pérez1https://orcid.org/0000-0002-1199-9564Carolina Agurto-Gangas2https://orcid.org/0000-0002-7238-2306Anibal Sierra3https://orcid.org/0000-0002-5991-8073Leon Trapman4https://orcid.org/0000-0002-8623-9703Miguel Vioque5https://orcid.org/0000-0002-4147-3846Nicolas Kurtovic6https://orcid.org/0000-0002-2358-4796Paola Pinilla7https://orcid.org/0000-0001-8764-1780Ilaria Pascucci8https://orcid.org/0000-0001-7962-1683Ke Zhang9https://orcid.org/0000-0002-0661-7517Rossella Anania10https://orcid.org/0009-0004-8091-5055John Carpenter11https://orcid.org/0000-0003-2251-0602Lucas A. Cieza12https://orcid.org/0000-0002-2828-1153Dingshan Deng13https://orcid.org/0000-0003-0777-7392Camilo González-Ruilova14https://orcid.org/0000-0003-4907-189XGiovanni P. Rosotti15https://orcid.org/0000-0003-4853-5736Dary A. Ruiz-Rodriguez16https://orcid.org/0000-0003-3573-8163Estephani E. TorresVillanueva17https://orcid.org/0000-0001-9961-8203Departamento de Física, Universidad de Santiago de Chile , Av. Victor Jara 3659, Santiago, Chile; Millennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Center for Interdisciplinary Research in Astrophysics Space Exploration (CIRAS) , Universidad de Santiago de Chile, ChileDepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileDepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileDepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, Chile; Mullard Space Science Laboratory, University College London , Holmbury St Mary, Dorking, Surrey RH5 6NT, UKDepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USAEuropean Southern Observatory , Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany; Joint ALMA Observatory , Avenida Alonso de Córdova 3107, Vitacura, Santiago, ChileMax-Planck-Institut fur Astronomie (MPIA) , Konigstuhl 17, 69117 Heidelberg, GermanyMullard Space Science Laboratory, University College London , Holmbury St Mary, Dorking, Surrey RH5 6NT, UKLunar and Planetary Laboratory, The University of Arizona , Tucson, AZ 85721, USADepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USADipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, I-20133 Milano, ItalyJoint ALMA Observatory , Avenida Alonso de Córdova 3107, Vitacura, Santiago, ChileMillennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Instituto de Estudios Astrofísicos, Universidad Diego Portales , Av. Ejercito 441, Santiago, ChileLunar and Planetary Laboratory, The University of Arizona , Tucson, AZ 85721, USAMillennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Center for Interdisciplinary Research in Astrophysics Space Exploration (CIRAS) , Universidad de Santiago de Chile, Chile; Instituto de Estudios Astrofísicos, Universidad Diego Portales , Av. Ejercito 441, Santiago, ChileDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, I-20133 Milano, ItalyJoint ALMA Observatory , Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile; National Radio Astronomy Observatory, 520 Edgemont Road , Charlottesville, VA 22903, USADepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USAVariability of millimeter wavelength continuum emission from Class II protoplanetary disks is extremely rare, and when detected, it is usually interpreted as originating from nonthermal emission mechanisms that relate to the host star itself rather than its disk. During observations made as part of the AGE-PRO Large Program, significant variability in the brightness of the 2MASS J16202863-2442087 system was detected between individual executions. We report the observed properties of the variability detected at millimeter wavelengths and investigate potential driving mechanisms. To investigate the nature of the variability, we construct a light curve from the continuum observations and analyze images constructed from both flaring and quiescent emission. We characterize the dust disk around the star through analysis in the image and visibility plane, and carry out kinematic analysis of CO (2–1) emission from the gas disk. The continuum flux decays by a factor of 8 in less than an hour, and by a factor of 13 within 8 days. The peak brightness coincides with an expected brightness maximum extrapolated from the periodicity of previously observed optical variability. The flare is most likely the product of synchrotron emission in the close vicinity of the star. The nature of the millimeter flare closely resembles those detected in very close binary systems, and may be due to the interaction of magnetic fields in an as-yet undetected binary. Alternatively, if the central host is a single-star object, the flare may be due to the interaction of magnetic field loops at the stellar surface or a strong accretion burst.https://doi.org/10.3847/1538-4357/add25cProtoplanetary disksVariable starsLow mass stars |
| spellingShingle | James M. Miley Laura M. Pérez Carolina Agurto-Gangas Anibal Sierra Leon Trapman Miguel Vioque Nicolas Kurtovic Paola Pinilla Ilaria Pascucci Ke Zhang Rossella Anania John Carpenter Lucas A. Cieza Dingshan Deng Camilo González-Ruilova Giovanni P. Rosotti Dary A. Ruiz-Rodriguez Estephani E. TorresVillanueva The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II Disk The Astrophysical Journal Protoplanetary disks Variable stars Low mass stars |
| title | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II Disk |
| title_full | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II Disk |
| title_fullStr | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II Disk |
| title_full_unstemmed | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II Disk |
| title_short | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). XII. Extreme Millimeter Variability Detected in a Class II Disk |
| title_sort | alma survey of gas evolution of protoplanetary disks age pro xii extreme millimeter variability detected in a class ii disk |
| topic | Protoplanetary disks Variable stars Low mass stars |
| url | https://doi.org/10.3847/1538-4357/add25c |
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