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Title: 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

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{sup −7}–10{sup −8} M {sub ⊙}, on massive white dwarfs. Such binaries include, but are not limited to, the recurrent novae. These same models predict the existencemore » of ultrafast novae that display decline times, t {sub 2,} to be as short as five hours. We outline a strategy for their future detection.« less

Authors:
; ;  [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [9];  [10]
  1. Department of Astrophysics, American Museum of Natural History, Central Park West and 79th Street, New York, NY 10024-5192 (United States)
  2. National Optical Astronomy Observatory, P.O. Box 26732, Tucson, AZ 85726 (United States)
  3. KIPAC, SLAC, 2575 Sand Hill Road, M/S 29, Menlo Park, CA 94025 (United States)
  4. School of Physics and Astronomy, Faculty of Exact Sciences, Tel Aviv University, Tel Aviv (Israel)
  5. CSIRO, Astronomy and Space Science, P.O. Box 76, Epping, NSW 1710 (Australia)
  6. N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL 00-716 Warsaw (Poland)
  7. California Institute of Technology, 1200 East California Boulevard, MC 278-17, Pasadena CA 91125 (United States)
  8. Department of Geosciences, Tel Aviv University, Ramat Aviv, Tel Aviv 69978 (Israel)
  9. Department of Physics and Astronomy, McMaster University, Hamilton, L8S 4M1, Ontario (Canada)
  10. Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 76100 Rehovot (Israel)
Publication Date:
OSTI Identifier:
22663687
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 839; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COMPUTERIZED SIMULATION; DETECTION; FORECASTING; GALAXIES; MASS; NOVAE; SPACE; STELLAR FLARES; TELESCOPES; WHITE DWARF STARS

Citation Formats

Shara, Michael M., Doyle, Trisha, Zurek, David, Lauer, Tod R., Baltz, Edward A., Kovetz, Attay, Madrid, Juan P., Mikołajewska, Joanna, Neill, J. D., Prialnik, Dina, Welch, D. L., and Yaron, Ofer. 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. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA65CD.
Shara, Michael M., Doyle, Trisha, Zurek, David, Lauer, Tod R., Baltz, Edward A., Kovetz, Attay, Madrid, Juan P., Mikołajewska, Joanna, Neill, J. D., Prialnik, Dina, Welch, D. L., & Yaron, Ofer. 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. United States. doi:10.3847/1538-4357/AA65CD.
Shara, Michael M., Doyle, Trisha, Zurek, David, Lauer, Tod R., Baltz, Edward A., Kovetz, Attay, Madrid, Juan P., Mikołajewska, Joanna, Neill, J. D., Prialnik, Dina, Welch, D. L., and Yaron, Ofer. Thu . "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". United States. doi:10.3847/1538-4357/AA65CD.
@article{osti_22663687,
title = {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},
author = {Shara, Michael M. and Doyle, Trisha and Zurek, David and Lauer, Tod R. 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},
abstractNote = {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{sup −7}–10{sup −8} M {sub ⊙}, 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 {sub 2,} to be as short as five hours. We outline a strategy for their future detection.},
doi = {10.3847/1538-4357/AA65CD},
journal = {Astrophysical Journal},
number = 2,
volume = 839,
place = {United States},
year = {Thu Apr 20 00:00:00 EDT 2017},
month = {Thu Apr 20 00:00:00 EDT 2017}
}