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  • 1310.0949v1

    Rights statement: This is an author-created, un-copyedited version of an article accepted for publication/published in Nanotechnology. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.1088/2041-8205/777/2/L32

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Rapid dust formation in novae: the speed-class formation timescale correlation eplained

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Rapid dust formation in novae : the speed-class formation timescale correlation eplained. / Williams, S. C.; Bode, M. F.; Darnley, M. J.; Evans, A.; Zubko, V.; Shafter, A. W.

In: Astrophysical Journal Letters, Vol. 777, No. 2, L32, 25.10.2013.

Research output: Contribution to journalJournal articlepeer-review

Harvard

Williams, SC, Bode, MF, Darnley, MJ, Evans, A, Zubko, V & Shafter, AW 2013, 'Rapid dust formation in novae: the speed-class formation timescale correlation eplained', Astrophysical Journal Letters, vol. 777, no. 2, L32. https://doi.org/10.1088/2041-8205/777/2/L32

APA

Williams, S. C., Bode, M. F., Darnley, M. J., Evans, A., Zubko, V., & Shafter, A. W. (2013). Rapid dust formation in novae: the speed-class formation timescale correlation eplained. Astrophysical Journal Letters, 777(2), [L32]. https://doi.org/10.1088/2041-8205/777/2/L32

Vancouver

Williams SC, Bode MF, Darnley MJ, Evans A, Zubko V, Shafter AW. Rapid dust formation in novae: the speed-class formation timescale correlation eplained. Astrophysical Journal Letters. 2013 Oct 25;777(2). L32. https://doi.org/10.1088/2041-8205/777/2/L32

Author

Williams, S. C. ; Bode, M. F. ; Darnley, M. J. ; Evans, A. ; Zubko, V. ; Shafter, A. W. / Rapid dust formation in novae : the speed-class formation timescale correlation eplained. In: Astrophysical Journal Letters. 2013 ; Vol. 777, No. 2.

Bibtex

@article{5b907f17d9704bcc8daf4428893b3b06,
title = "Rapid dust formation in novae: the speed-class formation timescale correlation eplained",
abstract = "Observations show that the time of onset of dust formation in classical novae depends strongly on their speed class, with dust typically taking longer to form in slower novae. Using empirical relationships between speed class, luminosity and ejection velocity, it can be shown that dust formation timescale is expected to be essentially independent of speed class. However, following a nova outburst the spectrum of the central hot source evolves, with an increasing proportion of the radiation being emitted short-ward of the Lyman limit. The rate at which the spectrum evolves also depends on the speed class. We have therefore refined the simple model by assuming photons at energies higher than the Lyman limit are absorbed by neutral hydrogen gas internal to the dust formation sites, therefore preventing these photons reaching the nucleation sites. With this refinement the dust formation timescale is theoretically dependent on speed class and the results of our theoretical modification agree well with the observational data. We consider two types of carbon-based dust, graphite and amorphous carbon, with both types producing similar relationships. Our results can be used to predict when dust will form in a nova of a given speed class and hence when observations should optimally be taken to detect the onset of dust formation.",
author = "Williams, {S. C.} and Bode, {M. F.} and Darnley, {M. J.} and A. Evans and V. Zubko and Shafter, {A. W.}",
note = "This is an author-created, un-copyedited version of an article accepted for publication/published in Nanotechnology. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.1088/2041-8205/777/2/L32",
year = "2013",
month = oct,
day = "25",
doi = "10.1088/2041-8205/777/2/L32",
language = "English",
volume = "777",
journal = "Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "IOP Publishing Ltd",
number = "2",

}

RIS

TY - JOUR

T1 - Rapid dust formation in novae

T2 - the speed-class formation timescale correlation eplained

AU - Williams, S. C.

AU - Bode, M. F.

AU - Darnley, M. J.

AU - Evans, A.

AU - Zubko, V.

AU - Shafter, A. W.

N1 - This is an author-created, un-copyedited version of an article accepted for publication/published in Nanotechnology. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.1088/2041-8205/777/2/L32

PY - 2013/10/25

Y1 - 2013/10/25

N2 - Observations show that the time of onset of dust formation in classical novae depends strongly on their speed class, with dust typically taking longer to form in slower novae. Using empirical relationships between speed class, luminosity and ejection velocity, it can be shown that dust formation timescale is expected to be essentially independent of speed class. However, following a nova outburst the spectrum of the central hot source evolves, with an increasing proportion of the radiation being emitted short-ward of the Lyman limit. The rate at which the spectrum evolves also depends on the speed class. We have therefore refined the simple model by assuming photons at energies higher than the Lyman limit are absorbed by neutral hydrogen gas internal to the dust formation sites, therefore preventing these photons reaching the nucleation sites. With this refinement the dust formation timescale is theoretically dependent on speed class and the results of our theoretical modification agree well with the observational data. We consider two types of carbon-based dust, graphite and amorphous carbon, with both types producing similar relationships. Our results can be used to predict when dust will form in a nova of a given speed class and hence when observations should optimally be taken to detect the onset of dust formation.

AB - Observations show that the time of onset of dust formation in classical novae depends strongly on their speed class, with dust typically taking longer to form in slower novae. Using empirical relationships between speed class, luminosity and ejection velocity, it can be shown that dust formation timescale is expected to be essentially independent of speed class. However, following a nova outburst the spectrum of the central hot source evolves, with an increasing proportion of the radiation being emitted short-ward of the Lyman limit. The rate at which the spectrum evolves also depends on the speed class. We have therefore refined the simple model by assuming photons at energies higher than the Lyman limit are absorbed by neutral hydrogen gas internal to the dust formation sites, therefore preventing these photons reaching the nucleation sites. With this refinement the dust formation timescale is theoretically dependent on speed class and the results of our theoretical modification agree well with the observational data. We consider two types of carbon-based dust, graphite and amorphous carbon, with both types producing similar relationships. Our results can be used to predict when dust will form in a nova of a given speed class and hence when observations should optimally be taken to detect the onset of dust formation.

U2 - 10.1088/2041-8205/777/2/L32

DO - 10.1088/2041-8205/777/2/L32

M3 - Journal article

VL - 777

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

SN - 2041-8205

IS - 2

M1 - L32

ER -