Multipoint Detection of GRB221009A’s Propagation through the Heliosphere
We present the results of processing the effects of the powerful gamma-ray burst GRB221009A captured by the charged particle detectors (electrostatic analyzers and solid-state detectors) on board spacecraft at different points in the heliosphere on 2022 October 9. To follow the GRB221009A propagatio...
| Main Authors: | , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Letters |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/2041-8213/acf933 |
| _version_ | 1827799237571641344 |
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| author | Andrii Voshchepynets Oleksiy V. Agapitov Lynn Wilson III Vassilis Angelopoulos Samer T. Alnussirat Michael Balikhin Myroslava Hlebena Ihor Korol Davin Larson David Mitchell Christopher Owen Ali Rahmati |
| author_facet | Andrii Voshchepynets Oleksiy V. Agapitov Lynn Wilson III Vassilis Angelopoulos Samer T. Alnussirat Michael Balikhin Myroslava Hlebena Ihor Korol Davin Larson David Mitchell Christopher Owen Ali Rahmati |
| author_sort | Andrii Voshchepynets |
| collection | DOAJ |
| description | We present the results of processing the effects of the powerful gamma-ray burst GRB221009A captured by the charged particle detectors (electrostatic analyzers and solid-state detectors) on board spacecraft at different points in the heliosphere on 2022 October 9. To follow the GRB221009A propagation through the heliosphere, we used the electron and proton flux measurements from solar missions Solar Orbiter and STEREO-A; Earth’s magnetosphere and solar wind missions THEMIS and Wind; meteorological satellites POES15, POES19, and MetOp3; and MAVEN—a NASA mission orbiting Mars. GRB221009A had a structure of four bursts: the less intense Pulse 1—the triggering impulse—was detected by gamma-ray observatories at T _0 = 13:16:59 UT (near the Earth); the most intense Pulses 2 and 3 were detected on board all the spacecraft from the list; and Pulse 4 was detected in more than 500 s after Pulse 1. Due to their different scientific objectives, the spacecraft, whose data were used in this study, were separated by more than 1 au (Solar Orbiter and MAVEN). This enabled the tracking of GRB221009A as it was propagating across the heliosphere. STEREO-A was the first to register Pulse 2 and 3 of the GRB, almost 100 s before their detection by spacecraft in the vicinity of Earth. MAVEN detected GRB221009A Pulses 2, 3, and 4 at the orbit of Mars about 237 s after their detection near Earth. By processing the observed time delays, we show that the source location of the GRB221009A was at R.A. 288.°5, decl. 18.°5 ± 2° (J2000). |
| first_indexed | 2024-03-11T19:48:42Z |
| format | Article |
| id | doaj.art-a726254acc144e4c97ed2e8451f0bcb6 |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-11T19:48:42Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj.art-a726254acc144e4c97ed2e8451f0bcb62023-10-05T15:57:49ZengIOP PublishingThe Astrophysical Journal Letters2041-82052023-01-019561L410.3847/2041-8213/acf933Multipoint Detection of GRB221009A’s Propagation through the HeliosphereAndrii Voshchepynets0https://orcid.org/0000-0001-8307-781XOleksiy V. Agapitov1https://orcid.org/0000-0001-6427-1596Lynn Wilson III2https://orcid.org/0000-0002-4313-1970Vassilis Angelopoulos3https://orcid.org/0000-0001-7024-1561Samer T. Alnussirat4https://orcid.org/0000-0001-6125-6411Michael Balikhin5https://orcid.org/0000-0002-8110-5626Myroslava Hlebena6https://orcid.org/0000-0003-1100-515XIhor Korol7https://orcid.org/0000-0001-7826-0249Davin Larson8https://orcid.org/0000-0001-5030-6030David Mitchell9https://orcid.org/0000-0001-9154-7236Christopher Owen10https://orcid.org/0000-0002-5982-4667Ali Rahmati11https://orcid.org/0000-0003-0519-6498Department of System Analysis and Optimization Theory, Uzhhorod National University , Uzhhorod, Ukraine; Space Sciences Laboratory, University of California , Berkeley, CA 94720, USASpace Sciences Laboratory, University of California , Berkeley, CA 94720, USA; Astronomy and Space Physics Department, National Taras Shevchenko University of Kyiv , Kyiv, UkraineGoddard Space Flight Center, National Aeronautics and Space Administration , Greenbelt, MD, USADepartment of Earth, Planetary, and Space Sciences, University of California , Los Angeles, CA, USASpace Sciences Laboratory, University of California , Berkeley, CA 94720, USAUniversity of Sheffield , Sheffield, UKDepartment of System Analysis and Optimization Theory, Uzhhorod National University , Uzhhorod, UkraineDepartment of Algebra and Differential Equation, Uzhhorod National University , Uzhhorod, Ukraine; Department of Mathematical Analysis, The John Paul II Catholic University of Lublin , Lublin, PolandSpace Sciences Laboratory, University of California , Berkeley, CA 94720, USASpace Sciences Laboratory, University of California , Berkeley, CA 94720, USAMullard Space Science Laboratory, University College London , Dorking RH5 6NT, UKSpace Sciences Laboratory, University of California , Berkeley, CA 94720, USAWe present the results of processing the effects of the powerful gamma-ray burst GRB221009A captured by the charged particle detectors (electrostatic analyzers and solid-state detectors) on board spacecraft at different points in the heliosphere on 2022 October 9. To follow the GRB221009A propagation through the heliosphere, we used the electron and proton flux measurements from solar missions Solar Orbiter and STEREO-A; Earth’s magnetosphere and solar wind missions THEMIS and Wind; meteorological satellites POES15, POES19, and MetOp3; and MAVEN—a NASA mission orbiting Mars. GRB221009A had a structure of four bursts: the less intense Pulse 1—the triggering impulse—was detected by gamma-ray observatories at T _0 = 13:16:59 UT (near the Earth); the most intense Pulses 2 and 3 were detected on board all the spacecraft from the list; and Pulse 4 was detected in more than 500 s after Pulse 1. Due to their different scientific objectives, the spacecraft, whose data were used in this study, were separated by more than 1 au (Solar Orbiter and MAVEN). This enabled the tracking of GRB221009A as it was propagating across the heliosphere. STEREO-A was the first to register Pulse 2 and 3 of the GRB, almost 100 s before their detection by spacecraft in the vicinity of Earth. MAVEN detected GRB221009A Pulses 2, 3, and 4 at the orbit of Mars about 237 s after their detection near Earth. By processing the observed time delays, we show that the source location of the GRB221009A was at R.A. 288.°5, decl. 18.°5 ± 2° (J2000).https://doi.org/10.3847/2041-8213/acf933Gamma-ray bursts |
| spellingShingle | Andrii Voshchepynets Oleksiy V. Agapitov Lynn Wilson III Vassilis Angelopoulos Samer T. Alnussirat Michael Balikhin Myroslava Hlebena Ihor Korol Davin Larson David Mitchell Christopher Owen Ali Rahmati Multipoint Detection of GRB221009A’s Propagation through the Heliosphere The Astrophysical Journal Letters Gamma-ray bursts |
| title | Multipoint Detection of GRB221009A’s Propagation through the Heliosphere |
| title_full | Multipoint Detection of GRB221009A’s Propagation through the Heliosphere |
| title_fullStr | Multipoint Detection of GRB221009A’s Propagation through the Heliosphere |
| title_full_unstemmed | Multipoint Detection of GRB221009A’s Propagation through the Heliosphere |
| title_short | Multipoint Detection of GRB221009A’s Propagation through the Heliosphere |
| title_sort | multipoint detection of grb221009a s propagation through the heliosphere |
| topic | Gamma-ray bursts |
| url | https://doi.org/10.3847/2041-8213/acf933 |
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