Breaking the Habit

The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a

M. Henze, M. Henze, M. J. Darnley, S. C. Williams, Mariko Kato, I. Hachisu, G. C. Anupama, A. Arai, D. Boyd, D. Burke, R. Ciardullo, K. Chinetti, L. M. Cook, M. J. Cook, P. Erdman, X. Gao, B. Harris, D. H. Hartmann, K. Hornoch, J. Chuck Horst & 54 others R. Hounsell, D. Husar, K. Itagaki, F. Kabashima, S. Kafka, A. Kaur, S. Kiyota, N. Kojiguchi, H. Kučáková, K. Kuramoto, H. Maehara, A. Mantero, F. J. Masci, K. Matsumoto, H. Naito, J. U. Ness, K. Nishiyama, A. Oksanen, J. P. Osborne, K. L. Page, E. Paunzen, M. Pavana, R. Pickard, J. Prieto-Arranz, P. Rodríguez-Gil, G. Sala, Y. Sano, A. W. Shafter, Y. Sugiura, H. Tan, T. Tordai, J. Vraštil, R. M. Wagner, F. Watanabe, B. F. Williams, M. F. Bode, A. Bruno, B. Buchheim, T. Crawford, B. Goff, M. Hernanz, A. S. Igarashi, J. José, M. Motta, T. J. O'Brien, T. Oswalt, G. Poyner, V. A.R.M. Ribeiro, R. Sabo, M. M. Shara, J. Shears, D. Starkey, S. Starrfield, C. E. Woodward

Research output: Contribution to journalArticle

5 Citations (Scopus)

Abstract

Since its discovery in 2008, the Andromeda galaxy nova M31N 2008-12a has been observed in eruption every single year. This unprecedented frequency indicates an extreme object, with a massive white dwarf and a high accretion rate, which is the most promising candidate for the single-degenerate progenitor of a Type Ia supernova known to date. The previous three eruptions of M31N 2008-12a have displayed remarkably homogeneous multiwavelength properties: (i) from a faint peak, the optical light curve declined rapidly by two magnitudes in less than two days, (ii) early spectra showed initial high velocities that slowed down significantly within days and displayed clear He/N lines throughout, and (iii) the supersoft X-ray source (SSS) phase of the nova began extremely early, six days after eruption, and only lasted for about two weeks. In contrast, the peculiar 2016 eruption was clearly different. Here we report (i) the considerable delay in the 2016 eruption date, (ii) the significantly shorter SSS phase, and (iii) the brighter optical peak magnitude (with a hitherto unobserved cusp shape). Early theoretical models suggest that these three different effects can be consistently understood as caused by a lower quiescence mass accretion rate. The corresponding higher ignition mass caused a brighter peak in the free-free emission model. The less massive accretion disk experienced greater disruption, consequently delaying the re-establishment of effective accretion. Without the early refueling, the SSS phase was shortened. Observing the next few eruptions will determine whether the properties of the 2016 outburst make it a genuine outlier in the evolution of M31N 2008-12a.

Original languageEnglish
Article number68
JournalAstrophysical Journal
Volume857
Issue number1
DOIs
Publication statusPublished - 2018 Apr 10

Fingerprint

habits
volcanic eruptions
volcanic eruption
accretion
Andromeda Galaxy
refueling
outlier
cusps
accretion disks
outburst
ignition
light curve
supernovae
x rays

Keywords

  • galaxies: individual (M31)
  • novae, cataclysmic variables
  • stars: individual (M31N 2008-12a)
  • ultraviolet: stars
  • X-rays: binaries

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Henze, M., Henze, M., Darnley, M. J., Williams, S. C., Kato, M., Hachisu, I., ... Woodward, C. E. (2018). Breaking the Habit: The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a. Astrophysical Journal, 857(1), [68]. https://doi.org/10.3847/1538-4357/aab6a6

Breaking the Habit : The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a. / Henze, M.; Henze, M.; Darnley, M. J.; Williams, S. C.; Kato, Mariko; Hachisu, I.; Anupama, G. C.; Arai, A.; Boyd, D.; Burke, D.; Ciardullo, R.; Chinetti, K.; Cook, L. M.; Cook, M. J.; Erdman, P.; Gao, X.; Harris, B.; Hartmann, D. H.; Hornoch, K.; Horst, J. Chuck; Hounsell, R.; Husar, D.; Itagaki, K.; Kabashima, F.; Kafka, S.; Kaur, A.; Kiyota, S.; Kojiguchi, N.; Kučáková, H.; Kuramoto, K.; Maehara, H.; Mantero, A.; Masci, F. J.; Matsumoto, K.; Naito, H.; Ness, J. U.; Nishiyama, K.; Oksanen, A.; Osborne, J. P.; Page, K. L.; Paunzen, E.; Pavana, M.; Pickard, R.; Prieto-Arranz, J.; Rodríguez-Gil, P.; Sala, G.; Sano, Y.; Shafter, A. W.; Sugiura, Y.; Tan, H.; Tordai, T.; Vraštil, J.; Wagner, R. M.; Watanabe, F.; Williams, B. F.; Bode, M. F.; Bruno, A.; Buchheim, B.; Crawford, T.; Goff, B.; Hernanz, M.; Igarashi, A. S.; José, J.; Motta, M.; O'Brien, T. J.; Oswalt, T.; Poyner, G.; Ribeiro, V. A.R.M.; Sabo, R.; Shara, M. M.; Shears, J.; Starkey, D.; Starrfield, S.; Woodward, C. E.

In: Astrophysical Journal, Vol. 857, No. 1, 68, 10.04.2018.

Research output: Contribution to journalArticle

Henze, M, Henze, M, Darnley, MJ, Williams, SC, Kato, M, Hachisu, I, Anupama, GC, Arai, A, Boyd, D, Burke, D, Ciardullo, R, Chinetti, K, Cook, LM, Cook, MJ, Erdman, P, Gao, X, Harris, B, Hartmann, DH, Hornoch, K, Horst, JC, Hounsell, R, Husar, D, Itagaki, K, Kabashima, F, Kafka, S, Kaur, A, Kiyota, S, Kojiguchi, N, Kučáková, H, Kuramoto, K, Maehara, H, Mantero, A, Masci, FJ, Matsumoto, K, Naito, H, Ness, JU, Nishiyama, K, Oksanen, A, Osborne, JP, Page, KL, Paunzen, E, Pavana, M, Pickard, R, Prieto-Arranz, J, Rodríguez-Gil, P, Sala, G, Sano, Y, Shafter, AW, Sugiura, Y, Tan, H, Tordai, T, Vraštil, J, Wagner, RM, Watanabe, F, Williams, BF, Bode, MF, Bruno, A, Buchheim, B, Crawford, T, Goff, B, Hernanz, M, Igarashi, AS, José, J, Motta, M, O'Brien, TJ, Oswalt, T, Poyner, G, Ribeiro, VARM, Sabo, R, Shara, MM, Shears, J, Starkey, D, Starrfield, S & Woodward, CE 2018, 'Breaking the Habit: The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a', Astrophysical Journal, vol. 857, no. 1, 68. https://doi.org/10.3847/1538-4357/aab6a6
Henze, M. ; Henze, M. ; Darnley, M. J. ; Williams, S. C. ; Kato, Mariko ; Hachisu, I. ; Anupama, G. C. ; Arai, A. ; Boyd, D. ; Burke, D. ; Ciardullo, R. ; Chinetti, K. ; Cook, L. M. ; Cook, M. J. ; Erdman, P. ; Gao, X. ; Harris, B. ; Hartmann, D. H. ; Hornoch, K. ; Horst, J. Chuck ; Hounsell, R. ; Husar, D. ; Itagaki, K. ; Kabashima, F. ; Kafka, S. ; Kaur, A. ; Kiyota, S. ; Kojiguchi, N. ; Kučáková, H. ; Kuramoto, K. ; Maehara, H. ; Mantero, A. ; Masci, F. J. ; Matsumoto, K. ; Naito, H. ; Ness, J. U. ; Nishiyama, K. ; Oksanen, A. ; Osborne, J. P. ; Page, K. L. ; Paunzen, E. ; Pavana, M. ; Pickard, R. ; Prieto-Arranz, J. ; Rodríguez-Gil, P. ; Sala, G. ; Sano, Y. ; Shafter, A. W. ; Sugiura, Y. ; Tan, H. ; Tordai, T. ; Vraštil, J. ; Wagner, R. M. ; Watanabe, F. ; Williams, B. F. ; Bode, M. F. ; Bruno, A. ; Buchheim, B. ; Crawford, T. ; Goff, B. ; Hernanz, M. ; Igarashi, A. S. ; José, J. ; Motta, M. ; O'Brien, T. J. ; Oswalt, T. ; Poyner, G. ; Ribeiro, V. A.R.M. ; Sabo, R. ; Shara, M. M. ; Shears, J. ; Starkey, D. ; Starrfield, S. ; Woodward, C. E. / Breaking the Habit : The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a. In: Astrophysical Journal. 2018 ; Vol. 857, No. 1.
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abstract = "Since its discovery in 2008, the Andromeda galaxy nova M31N 2008-12a has been observed in eruption every single year. This unprecedented frequency indicates an extreme object, with a massive white dwarf and a high accretion rate, which is the most promising candidate for the single-degenerate progenitor of a Type Ia supernova known to date. The previous three eruptions of M31N 2008-12a have displayed remarkably homogeneous multiwavelength properties: (i) from a faint peak, the optical light curve declined rapidly by two magnitudes in less than two days, (ii) early spectra showed initial high velocities that slowed down significantly within days and displayed clear He/N lines throughout, and (iii) the supersoft X-ray source (SSS) phase of the nova began extremely early, six days after eruption, and only lasted for about two weeks. In contrast, the peculiar 2016 eruption was clearly different. Here we report (i) the considerable delay in the 2016 eruption date, (ii) the significantly shorter SSS phase, and (iii) the brighter optical peak magnitude (with a hitherto unobserved cusp shape). Early theoretical models suggest that these three different effects can be consistently understood as caused by a lower quiescence mass accretion rate. The corresponding higher ignition mass caused a brighter peak in the free-free emission model. The less massive accretion disk experienced greater disruption, consequently delaying the re-establishment of effective accretion. Without the early refueling, the SSS phase was shortened. Observing the next few eruptions will determine whether the properties of the 2016 outburst make it a genuine outlier in the evolution of M31N 2008-12a.",
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T2 - The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a

AU - Henze, M.

AU - Henze, M.

AU - Darnley, M. J.

AU - Williams, S. C.

AU - Kato, Mariko

AU - Hachisu, I.

AU - Anupama, G. C.

AU - Arai, A.

AU - Boyd, D.

AU - Burke, D.

AU - Ciardullo, R.

AU - Chinetti, K.

AU - Cook, L. M.

AU - Cook, M. J.

AU - Erdman, P.

AU - Gao, X.

AU - Harris, B.

AU - Hartmann, D. H.

AU - Hornoch, K.

AU - Horst, J. Chuck

AU - Hounsell, R.

AU - Husar, D.

AU - Itagaki, K.

AU - Kabashima, F.

AU - Kafka, S.

AU - Kaur, A.

AU - Kiyota, S.

AU - Kojiguchi, N.

AU - Kučáková, H.

AU - Kuramoto, K.

AU - Maehara, H.

AU - Mantero, A.

AU - Masci, F. J.

AU - Matsumoto, K.

AU - Naito, H.

AU - Ness, J. U.

AU - Nishiyama, K.

AU - Oksanen, A.

AU - Osborne, J. P.

AU - Page, K. L.

AU - Paunzen, E.

AU - Pavana, M.

AU - Pickard, R.

AU - Prieto-Arranz, J.

AU - Rodríguez-Gil, P.

AU - Sala, G.

AU - Sano, Y.

AU - Shafter, A. W.

AU - Sugiura, Y.

AU - Tan, H.

AU - Tordai, T.

AU - Vraštil, J.

AU - Wagner, R. M.

AU - Watanabe, F.

AU - Williams, B. F.

AU - Bode, M. F.

AU - Bruno, A.

AU - Buchheim, B.

AU - Crawford, T.

AU - Goff, B.

AU - Hernanz, M.

AU - Igarashi, A. S.

AU - José, J.

AU - Motta, M.

AU - O'Brien, T. J.

AU - Oswalt, T.

AU - Poyner, G.

AU - Ribeiro, V. A.R.M.

AU - Sabo, R.

AU - Shara, M. M.

AU - Shears, J.

AU - Starkey, D.

AU - Starrfield, S.

AU - Woodward, C. E.

PY - 2018/4/10

Y1 - 2018/4/10

N2 - Since its discovery in 2008, the Andromeda galaxy nova M31N 2008-12a has been observed in eruption every single year. This unprecedented frequency indicates an extreme object, with a massive white dwarf and a high accretion rate, which is the most promising candidate for the single-degenerate progenitor of a Type Ia supernova known to date. The previous three eruptions of M31N 2008-12a have displayed remarkably homogeneous multiwavelength properties: (i) from a faint peak, the optical light curve declined rapidly by two magnitudes in less than two days, (ii) early spectra showed initial high velocities that slowed down significantly within days and displayed clear He/N lines throughout, and (iii) the supersoft X-ray source (SSS) phase of the nova began extremely early, six days after eruption, and only lasted for about two weeks. In contrast, the peculiar 2016 eruption was clearly different. Here we report (i) the considerable delay in the 2016 eruption date, (ii) the significantly shorter SSS phase, and (iii) the brighter optical peak magnitude (with a hitherto unobserved cusp shape). Early theoretical models suggest that these three different effects can be consistently understood as caused by a lower quiescence mass accretion rate. The corresponding higher ignition mass caused a brighter peak in the free-free emission model. The less massive accretion disk experienced greater disruption, consequently delaying the re-establishment of effective accretion. Without the early refueling, the SSS phase was shortened. Observing the next few eruptions will determine whether the properties of the 2016 outburst make it a genuine outlier in the evolution of M31N 2008-12a.

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KW - galaxies: individual (M31)

KW - novae, cataclysmic variables

KW - stars: individual (M31N 2008-12a)

KW - ultraviolet: stars

KW - X-rays: binaries

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