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; M. 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; 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

doi:10.3847/1538-4357/aab6a6

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, M. 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 HorstR. 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

Minnesota Institute for Astrophysics

Research output: Contribution to journal › Article › peer-review

26 Scopus citations

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 language	English (US)
Article number	68
Journal	Astrophysical Journal
Volume	857
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/aab6a6
State	Published - Apr 10 2018

Bibliographical note

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© 2018. The American Astronomical Society. All rights reserved.

Keywords

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

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

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

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title = "Breaking the Habit: The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a",

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.",

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

author = "M. Henze and M. Henze and Darnley, {M. J.} and Williams, {S. C.} and M. Kato and I. Hachisu and Anupama, {G. C.} and A. Arai and D. Boyd and D. Burke and R. Ciardullo and K. Chinetti and Cook, {L. M.} and Cook, {M. J.} and P. Erdman and X. Gao and B. Harris and Hartmann, {D. H.} and K. Hornoch and Horst, {J. Chuck} and R. Hounsell and D. Husar and K. Itagaki and F. Kabashima and S. Kafka and A. Kaur and S. Kiyota and N. Kojiguchi and H. Ku{\v c}{\'a}kov{\'a} and K. Kuramoto and H. Maehara and A. Mantero and Masci, {F. J.} and K. Matsumoto and H. Naito and Ness, {J. U.} and K. Nishiyama and A. Oksanen and Osborne, {J. P.} and Page, {K. L.} and E. Paunzen and M. Pavana and R. Pickard and J. Prieto-Arranz and P. Rodr{\'i}guez-Gil and G. Sala and Y. Sano and Shafter, {A. W.} and Y. Sugiura and H. Tan and T. Tordai and J. Vra{\v s}til and Wagner, {R. M.} and F. Watanabe and Williams, {B. F.} and Bode, {M. F.} and A. Bruno and B. Buchheim and T. Crawford and B. Goff and M. Hernanz and Igarashi, {A. S.} and J. Jos{\'e} and M. Motta and O'Brien, {T. J.} and T. Oswalt and G. Poyner and Ribeiro, {V. A.R.M.} and R. Sabo and Shara, {M. M.} and J. Shears and D. Starkey and S. Starrfield and Woodward, {C. E.}",

year = "2018",

month = apr,

day = "10",

doi = "10.3847/1538-4357/aab6a6",

language = "English (US)",

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journal = "Astrophysical Journal",

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TY - JOUR

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T2 - The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a

AU - Henze, M.

AU - Darnley, M. J.

AU - Williams, S. C.

AU - Kato, M.

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.

AB - 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.

KW - X-rays: binaries

KW - galaxies: individual (M31)

KW - novae, cataclysmic variables

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

KW - ultraviolet: stars

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JO - Astrophysical Journal

JF - Astrophysical Journal

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ER -

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

Abstract

Bibliographical note

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