The multiwavelength view of shocks in the fastest nova V1674 Her

Author:

Sokolovsky K V12ORCID,Johnson T J3ORCID,Buson S4ORCID,Jean P56ORCID,Cheung C C7ORCID,Mukai K8ORCID,Chomiuk L2ORCID,Aydi E2ORCID,Molina B2,Kawash A2ORCID,Linford J D9ORCID,Mioduszewski A J9,Rupen M P10,Sokoloski J L11,Williams M N9,Steinberg E12ORCID,Vurm I13ORCID,Metzger B D1114ORCID,Page K L15ORCID,Orio M1617ORCID,Quimby R M1819ORCID,Shafter A W18ORCID,Corbett H20ORCID,Bolzoni S2122ORCID,DeYoung J21,Menzies K21,Romanov F D2122ORCID,Richmond M23,Ulowetz J24,Vanmunster T212526,Williamson G21,Lane D J2721ORCID,Bartnik M2,Bellaver M2,Bruinsma E2,Dugan E2,Fedewa J2,Gerhard C2,Painter S2,Peterson D-M2,Rodriguez J E2ORCID,Smith C2,Sullivan H2,Watson S2

Affiliation:

1. Department of Astronomy, University of Illinois at Urbana-Champaign , 1002 W. Green Street, Urbana, IL 61801, USA

2. Department of Physics and Astronomy, Michigan State University , 567 Wilson Road, East Lansing, MI 48824, USA

3. College of Science, George Mason University , Fairfax, VA 22030, USA

4. Lehrstuhl für Astronomie, Universität Würzburg , Emil-Fischer-Street 31, D-Würzburg 97074, Germany

5. CNRS, IRAP , F-31028 Toulouse CEDEX 4, France

6. GAHEC, Université de Toulouse, UPS-OMP, IRAP , F-31400 Toulouse, France

7. Space Science Division, Naval Research Laboratory , Washington, DC 20375-5352, USA

8. CRESST and X-ray Astrophysics Laboratory , NASA/GSFC, Greenbelt, MD 20771, USA

9. National Radio Astronomy Observatory, Domenici Science Operations Center , 1003 Lopezville Road, Socorro, NM 87801, USA

10. National Research Council, Herzberg Astronomy and Astrophysics , 717 White Lake Road, PO Box 248, Penticton, BC V2A 6J9, Canada

11. Department of Physics and Columbia Astrophysics Laboratory, Columbia University , New York, NY 10027, USA

12. Racah Institute of Physics, The Hebrew University , 9190401 Jerusalem, Israel

13. Tartu Observatory, University of Tartu , Tõravere, 61602 Tartumaa, Estonia

14. Center for Computational Astrophysics, Flatiron Institute , 162 5th Avenue, New York, NY 10010, USA

15. School of Physics & Astronomy, University of Leicester , Leicester LE1 7RH, UK

16. Department of Astronomy, University of Wisconsin–Madison , 475 N. Charter Street, Madison, WI 53706, USA

17. INAF – Padova , vicolo Osservatorio, 5, I-35122 Padova, Italy

18. Department of Astronomy and Mount Laguna Observatory, San Diego State University , San Diego, CA 92182, USA

19. Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo , Kashiwa, Chiba 277-8583, Japan

20. Department of Physics and Astronomy, University of North Carolina at Chapel Hill , Chapel Hill, NC 27599-3255, USA

21. AAVSO Observer

22. Remote observer of Burke-Gaffney Observatory, Abbey Ridge Observatory and Mini-Robotic Observatory , Canada

23. School of Physics and Astronomy, Rochester Institute of Technology , 84 Lomb Memorial Drive, Rochester, NY 14623, USA

24. Center for Backyard Astrophysics Illinois, Northbrook Meadow Observatory , 855 Fair Ln, Northbrook, IL 60062, USA

25. Center for Backyard Astrophysics Belgium , Walhostraat 1a, B-3401 Landen, Belgium

26. Center for Backyard Astrophysics Extremadura , e-EyE Astronomical Complex, E-06340 Fregenal de la Sierra, Spain

27. Burke-Gaffney Observatory, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, Canada

Abstract

ABSTRACTClassical 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.

Funder

National Aeronautics and Space Administration

Ministry of Education, Culture, Sports, Science and Technology

Japan Aerospace Exploration Agency

Swedish Research Council

Istituto Nazionale di Astrofisica

DOE

National Science Foundation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 4 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

1. Soft X-ray and FUV observations of Nova Her 2021 (V1674 Her) with AstroSat;Monthly Notices of the Royal Astronomical Society;2023-12-18

2. Revisiting the classics: on the evolutionary origin of the ‘Fe ii’ and ‘He/N’ spectral classes of novae;Monthly Notices of the Royal Astronomical Society;2023-11-08

3. The RS Oph Outburst of 2021 Monitored in X-Rays with NICER;The Astrophysical Journal;2023-09-01

4. Antistars as possible sources of antihelium cosmic rays;Journal of Cosmology and Astroparticle Physics;2023-08-01

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