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A Hubble Space Telescope Survey for Novae in M87. II. Snuffing out the Maximum Magnitude–Rate of Decline Relation for Novae as a Non-standard Candle, and a Prediction of the Existence of Ultrafast Novae

Shara, Michael M. and Doyle, Trisha and Lauer, Tod R. and Zurek, David and Baltz, Edward A. and Kovetz, Attay and Madrid, Juan P. and Mikołajewska, Joanna and Neill, J. D. and Prialnik, Dina and Welch, D. L. and Yaron, Ofer (2017) A Hubble Space Telescope Survey for Novae in M87. II. Snuffing out the Maximum Magnitude–Rate of Decline Relation for Novae as a Non-standard Candle, and a Prediction of the Existence of Ultrafast Novae. Astrophysical Journal, 839 (2). Art. No. 109. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170421-151346490

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Abstract

The extensive grid of numerical simulations of nova eruptions from the work of Yaron et al. first predicted that some classical novae might significantly deviate from the Maximum Magnitude–Rate of Decline (MMRD) relation, which purports to characterize novae as standard candles. Kasliwal et al. have announced the observational detection of a new class of faint, fast classical novae in the Andromeda galaxy. These objects deviate strongly from the MMRD relationship, as predicted by Yaron et al. Recently, Shara et al. reported the first detections of faint, fast novae in M87. These previously overlooked objects are as common in the giant elliptical galaxy M87 as they are in the giant spiral M31; they comprise about 40% of all classical nova eruptions and greatly increase the observational scatter in the MMRD relation. We use the extensive grid of the nova simulations of Yaron et al. to identify the underlying causes of the existence of faint, fast novae. These are systems that have accreted, and can thus eject, only very low-mass envelopes, of the order of 10^(−7)–10^(−8) M_⊙, on massive white dwarfs. Such binaries include, but are not limited to, the recurrent novae. These same models predict the existence of ultrafast novae that display decline times, t_2, to be as short as five hours. We outline a strategy for their future detection.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa65cdDOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa65cd/metaPublisherArticle
https://arxiv.org/abs/1702.05788arXivDiscussion Paper
ORCID:
AuthorORCID
Doyle, Trisha0000-0001-7182-5307
Neill, J. D.0000-0002-0466-1119
Additional Information:© 2017 American Astronomical Society. Received 2015 December 24. Accepted 2016 May 1. Published 2017 April 21. We are grateful to A. Juodagalvis for providing the data of electron capture rates on heavy nuclei. H.N. acknowledges to M. Shibata, Y. Sekiguchi and H. Okawa for valuable comments and discussions. H.N. also thanks Werner Marcus for proofreadings. The numerical computations were performed on the supercomputers at K, at AICS, FX10 at Information Technology Center of Tokyo University, SR16000 at YITP of Kyoto University, and SR16000 at KEK under the support of its Large Scale Simulation Program (14/15-17, 15/16-08), Research Center for Nuclear Physics (RCNP) at Osaka University. Large-scale storage of numerical data is supported by JLDG constructed over SINET4 of NII. H.N. was supported in part by JSPS Postdoctoral Fellowships for Research Abroad No. 27-348. This work was also supported by Grant-in-Aid for the Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan (15K05093, 24103006, 24740165, 24244036, 25870099) and HPCI Strategic Program of Japanese MEXT and K computer at the RIKEN (Project ID: hpci 130025, 140211, and 150225).
Group:Space Astrophysics Laboratory
Funders:
Funding AgencyGrant Number
High Energy Accelerator Research Organization (KEK)14/15-17
High Energy Accelerator Research Organization (KEK)15/16-08
Osaka University Research Center for Nuclear PhysicsUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)27-348
Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) Japan15K05093
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24103006
Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan 24740165
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24244036
Ministry of Education, Culture, Sports, Science and Technology (MEXT)25870099
RIKEN130025
RIKEN140211
RIKEN150225
Subject Keywords:methods: numerical; neutrinos; radiative transfer; relativistic processes; (stars: supernovae: general)
Issue or Number:2
Record Number:CaltechAUTHORS:20170421-151346490
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170421-151346490
Official Citation:Michael M. Shara et al 2017 ApJ 839 109
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:76828
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:24 Apr 2017 16:38
Last Modified:03 Oct 2019 17:50

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