Discovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal Shocks
We present a detailed analysis of an extragalactic slow classical nova in M31 exhibiting multiple peaks in its light curve. Spectroscopic and photometric observations were used to investigate the underlying physical processes. Shock-induced heating events resulting in the expansion and contraction o...
Saved in:
| Main Authors: | , , , , , , , , , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ada5fe |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1825206165161639936 |
|---|---|
| author | Judhajeet Basu Ravi Kumar G.C. Anupama Sudhanshu Barway Peter H. Hauschildt Shatakshi Chamoli Vishwajeet Swain Varun Bhalero Viraj Karambelkar Mansi Kasliwal Kaustav K. Das Igor Andreoni Avinash Singh Rishabh Singh Teja |
| author_facet | Judhajeet Basu Ravi Kumar G.C. Anupama Sudhanshu Barway Peter H. Hauschildt Shatakshi Chamoli Vishwajeet Swain Varun Bhalero Viraj Karambelkar Mansi Kasliwal Kaustav K. Das Igor Andreoni Avinash Singh Rishabh Singh Teja |
| author_sort | Judhajeet Basu |
| collection | DOAJ |
| description | We present a detailed analysis of an extragalactic slow classical nova in M31 exhibiting multiple peaks in its light curve. Spectroscopic and photometric observations were used to investigate the underlying physical processes. Shock-induced heating events resulting in the expansion and contraction of the photosphere are likely responsible for the observed multiple peaks. Deviation of the observed spectrum at the peak from the models also suggests the presence of shocks. The successive peaks occurring at increasing intervals could be due to the series of internal shocks generated near or within the photosphere. Spectral modeling suggests a low-mass white dwarf (WD) accreting slowly from a companion star. The ejecta mass, estimated from spectral analysis, is ~10 ^−4 M _⊙ , which is typical for a slow nova. We estimate the binary, by comparing the archival Hubble Space Telescope data and eruption properties with stellar and nova models, to comprise a 0.65 M _⊙ primary WD and a K iii cool evolved secondary star. |
| format | Article |
| id | doaj-art-86dc0259f1ef477e90dfb7253820af17 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-86dc0259f1ef477e90dfb7253820af172025-02-07T12:00:49ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01980112910.3847/1538-4357/ada5feDiscovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal ShocksJudhajeet Basu0https://orcid.org/0000-0001-7570-545XRavi Kumar1https://orcid.org/0009-0008-6428-7668G.C. Anupama2https://orcid.org/0000-0003-3533-7183Sudhanshu Barway3https://orcid.org/0000-0002-3927-5402Peter H. Hauschildt4https://orcid.org/0000-0002-8077-5572Shatakshi Chamoli5https://orcid.org/0009-0000-5909-293XVishwajeet Swain6https://orcid.org/0000-0002-7942-8477Varun Bhalero7https://orcid.org/0000-0002-6112-7609Viraj Karambelkar8https://orcid.org/0000-0003-2758-159XMansi Kasliwal9https://orcid.org/0000-0002-5619-4938Kaustav K. Das10https://orcid.org/0000-0001-8372-997XIgor Andreoni11https://orcid.org/0000-0002-8977-1498Avinash Singh12https://orcid.org/0000-0003-2091-622XRishabh Singh Teja13https://orcid.org/0000-0002-0525-0872Indian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; judhajeet.basu@iiap.res.in, judhajeet20@gmail.com; Pondicherry University , R.V. Nagar, Kalapet, Pondicherry 605014, IndiaDepartment of Aerospace Engineering, Indian Institute of Technology Bombay , Powai, Mumbai 400076, IndiaIndian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; judhajeet.basu@iiap.res.in, judhajeet20@gmail.comIndian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; judhajeet.basu@iiap.res.in, judhajeet20@gmail.comHamburger Sternwarte, University of Hamburg , Gojenbergsweg 112, 21029 Hamburg, GermanyIndian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; judhajeet.basu@iiap.res.in, judhajeet20@gmail.com; Pondicherry University , R.V. Nagar, Kalapet, Pondicherry 605014, IndiaDepartment of Physics, Indian Institute of Technology Bombay , Powai, Mumbai 400076, IndiaDepartment of Physics, Indian Institute of Technology Bombay , Powai, Mumbai 400076, IndiaCahill Center for Astrophysics, California Institute of Technology , 1200 E. California Blvd., Pasadena, CA 91125, USACahill Center for Astrophysics, California Institute of Technology , 1200 E. California Blvd., Pasadena, CA 91125, USACahill Center for Astrophysics, California Institute of Technology , 1200 E. California Blvd., Pasadena, CA 91125, USADepartment of Physics and Astronomy, University of North Carolina at Chapel Hill , Chapel Hill, NC 27599-3255, USADepartment of Astronomy, The Oskar Klein Center, Stockholm University , AlbaNova University Center, SE 106 91 Stockholm, SwedenIndian Institute of Astrophysics , II Block, Koramangala, Bengaluru 560034, India ; judhajeet.basu@iiap.res.in, judhajeet20@gmail.com; Pondicherry University , R.V. Nagar, Kalapet, Pondicherry 605014, IndiaWe present a detailed analysis of an extragalactic slow classical nova in M31 exhibiting multiple peaks in its light curve. Spectroscopic and photometric observations were used to investigate the underlying physical processes. Shock-induced heating events resulting in the expansion and contraction of the photosphere are likely responsible for the observed multiple peaks. Deviation of the observed spectrum at the peak from the models also suggests the presence of shocks. The successive peaks occurring at increasing intervals could be due to the series of internal shocks generated near or within the photosphere. Spectral modeling suggests a low-mass white dwarf (WD) accreting slowly from a companion star. The ejecta mass, estimated from spectral analysis, is ~10 ^−4 M _⊙ , which is typical for a slow nova. We estimate the binary, by comparing the archival Hubble Space Telescope data and eruption properties with stellar and nova models, to comprise a 0.65 M _⊙ primary WD and a K iii cool evolved secondary star.https://doi.org/10.3847/1538-4357/ada5feClassical novaeAndromeda GalaxyShocksPhotometryLight curvesLight curve classification |
| spellingShingle | Judhajeet Basu Ravi Kumar G.C. Anupama Sudhanshu Barway Peter H. Hauschildt Shatakshi Chamoli Vishwajeet Swain Varun Bhalero Viraj Karambelkar Mansi Kasliwal Kaustav K. Das Igor Andreoni Avinash Singh Rishabh Singh Teja Discovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal Shocks The Astrophysical Journal Classical novae Andromeda Galaxy Shocks Photometry Light curves Light curve classification |
| title | Discovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal Shocks |
| title_full | Discovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal Shocks |
| title_fullStr | Discovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal Shocks |
| title_full_unstemmed | Discovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal Shocks |
| title_short | Discovery and Detailed Study of the M31 Classical Nova AT 2023tkw: Evidence for Internal Shocks |
| title_sort | discovery and detailed study of the m31 classical nova at 2023tkw evidence for internal shocks |
| topic | Classical novae Andromeda Galaxy Shocks Photometry Light curves Light curve classification |
| url | https://doi.org/10.3847/1538-4357/ada5fe |
| work_keys_str_mv | AT judhajeetbasu discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT ravikumar discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT gcanupama discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT sudhanshubarway discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT peterhhauschildt discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT shatakshichamoli discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT vishwajeetswain discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT varunbhalero discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT virajkarambelkar discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT mansikasliwal discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT kaustavkdas discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT igorandreoni discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT avinashsingh discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks AT rishabhsinghteja discoveryanddetailedstudyofthem31classicalnovaat2023tkwevidenceforinternalshocks |