| DOI | Resolve DOI: https://doi.org/10.1093/mnras/stad887 |
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| Author | Search for: Sokolovsky, K VORCID identifier: https://orcid.org/0000-0001-5991-6863; Search for: Johnson, T JORCID identifier: https://orcid.org/0000-0002-2771-472X; Search for: Buson, SORCID identifier: https://orcid.org/0000-0002-3308-324X; Search for: Jean, PORCID identifier: https://orcid.org/0000-0002-1757-9560; Search for: Cheung, C CORCID identifier: https://orcid.org/0000-0002-4377-0174; Search for: Mukai, KORCID identifier: https://orcid.org/0000-0002-8286-8094; Search for: Chomiuk, LORCID identifier: https://orcid.org/0000-0002-8400-3705; Search for: Aydi, EORCID identifier: https://orcid.org/0000-0001-8525-3442; Search for: Molina, B; Search for: Kawash, AORCID identifier: https://orcid.org/0000-0003-0071-1622; Search for: Linford, J DORCID identifier: https://orcid.org/0000-0002-3873-5497; Search for: Mioduszewski, A J; Search for: Rupen, M P1; Search for: Sokoloski, J L; Search for: Williams, M N; Search for: Steinberg, EORCID identifier: https://orcid.org/0000-0003-0053-0696; Search for: Vurm, IORCID identifier: https://orcid.org/0000-0003-1336-4746; Search for: Metzger, B DORCID identifier: https://orcid.org/0000-0002-4670-7509; Search for: Page, K LORCID identifier: https://orcid.org/0000-0001-5624-2613; Search for: Orio, MORCID identifier: https://orcid.org/0000-0003-1563-9803; Search for: Quimby, R MORCID identifier: https://orcid.org/0000-0001-9171-5236; Search for: Shafter, A WORCID identifier: https://orcid.org/0000-0002-1276-1486; Search for: Corbett, HORCID identifier: https://orcid.org/0000-0002-6339-6706; Search for: Bolzoni, SORCID identifier: https://orcid.org/0000-0003-0114-1318; Search for: DeYoung, J; Search for: Menzies, K; Search for: Romanov, F DORCID identifier: https://orcid.org/0000-0002-5268-7735; Search for: Richmond, M; Search for: Ulowetz, J; Search for: Vanmunster, T; Search for: Williamson, G; Search for: Lane, D JORCID identifier: https://orcid.org/0000-0002-6097-8719; Search for: Bartnik, M; Search for: Bellaver, M; Search for: Bruinsma, E; Search for: Dugan, E; Search for: Fedewa, J; Search for: Gerhard, C; Search for: Painter, S; Search for: Peterson, D-M; Search for: Rodriguez, J EORCID identifier: https://orcid.org/0000-0001-8812-0565; Search for: Smith, C; Search for: Sullivan, H; Search for: Watson, S |
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| Affiliation | - National Research Council of Canada. Herzberg Astronomy and Astrophysics
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| Funder | Search for: National Aeronautics and Space Administration; Search for: Ministry of Education, Culture, Sports, Science and Technology; Search for: Japan Aerospace Exploration Agency; Search for: Swedish Research Council; Search for: Istituto Nazionale di Astrofisica; Search for: DOE; Search for: National Science Foundation |
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| Format | Text, Article |
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| Subject | stars: individual: V1674 Her; novae; cataclysmic variables; white dwarfs; transients: novae |
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| Abstract | Classical novae are shock-powered multiwavelength transients triggered by a thermonuclear runaway on an accreting white dwarf. V1674 Her is the fastest nova ever recorded (time to declined by two magnitudes is t2 = 1.1 d) that challenges our understanding of shock formation in novae. We investigate the physical mechanisms behind nova emission from GeV γ-rays to cm-band radio using coordinated Fermi-LAT, NuSTAR, Swift, and VLA observations supported by optical photometry. Fermi-LAT detected short-lived (18 h) 0.1–100 GeV emission from V1674 Her that appeared 6 h after the eruption began; this was at a level of (1.6 ± 0.4) × 10⁻⁶ photons cm⁻² s⁻¹. Eleven days later, simultaneous NuSTAR and Swift X-ray observations revealed optically thin thermal plasma shock-heated to kTshock = 4 keV. The lack of a detectable 6.7 keV Fe Kα emission suggests super-solar CNO abundances. The radio emission from V1674 Her was consistent with thermal emission at early times and synchrotron at late times. The radio spectrum steeply rising with frequency may be a result of either free-free absorption of synchrotron and thermal emission by unshocked outer regions of the nova shell or the Razin–Tsytovich effect attenuating synchrotron emission in dense plasma. The development of the shock inside the ejecta is unaffected by the extraordinarily rapid evolution and the intermediate polar host of this nova. |
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| Publication date | 2023-03-23 |
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| Publisher | Oxford Academic |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 6b882c14-2bd7-434e-861d-9667ff82a8dd |
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| Record created | 2024-06-27 |
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| Record modified | 2024-06-27 |
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