Radio observations of the classical nova Cygni 92 eighty days after outburst

Pavelin, P. E.; Davis, R. J.; Morrison, L. V.; Bode, M. F.; Ivison, R. J.

doi:10.1038/363424a0

Cited by 45 publications

(12 citation statements)

References 3 publications

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“…First, we hold temperature fixed, as plotted in Figure 4. Brightness temperatures derived from spatially-resolved radio images of novae are in the range 10 4 -10 5 K (Taylor et al 1988;Pavelin et al 1993;Eyres et al 1996;Heywood et al 2005), consistent with a photoionized gas. Assuming a distance of 4.8 kpc, we obtain estimates of the photospheric radius for temperatures in this range (the difference between a 10 4 K and a 10 5 K photospheric radius is a constant factor of √ 10 ≈ 3.2).…”

Section: Evolution While T Pyx Is Optically Thick At Radiomentioning

confidence: 90%

The 2011 Outburst of Recurrent Nova T Pyx: Radio Observations Reveal the Ejecta Mass and Hint at Complex Mass Loss

Nelson

Chomiuk

Roy

et al. 2014

ApJ

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Despite being the prototype of its class, T Pyx is arguably the most unusual and poorly understood recurrent nova. Here, we use radio observations from the Karl G. Jansky Very Large Array to trace the evolution of the ejecta over the course of the 2011 outburst of T Pyx. The radio emission is broadly consistent with thermal emission from the nova ejecta. However, the radio flux began rising surprisingly late in the outburst, indicating that the bulk of the radio-emitting material was either very cold, or expanding very slowly, for the first ∼50 days of the outburst. Considering a plausible range of volume filling factors and geometries for the ejecta, we find that the high peak flux densities of the radio emission require a massive ejection of (1 − 30) × 10 −5 M ⊙ . This ejecta mass is much higher than the values normally associated with recurrent novae, and is more consistent with a nova on a white dwarf well below the Chandrasekhar limit.

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Section: Evolution While T Pyx Is Optically Thick At Radiomentioning

confidence: 90%

The 2011 Outburst of Recurrent Nova T Pyx: Radio Observations Reveal the Ejecta Mass and Hint at Complex Mass Loss

Nelson

Chomiuk

Roy

et al. 2014

ApJ

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“…Due to positional discrepancies of over 2 arcseconds the POSS pre-nova candidate may not be the true precursor (Pavelin et al 1993) which then implies a range of at least 16 magnitudes. We estimate the distance to the nova as 2.3 ± 0.5 kpc based on a simple average of optical interferometric and direct angular imaging, radio angular measures, and photometric measurements reported (Hayward et al 1992;Andrillat & Houziaux 1993;Barger et al 1993;Chochol1993;Paresce 1994;Pavelin et al 1993;Quirrenbach et al 1993). The nova is an ONeMg "neon nova" as suggested by or confirmed by many authors (Austin et al 1992;Shore et al 1992;Emerson & Mannings 1992).…”

Section: Introductionmentioning

confidence: 99%

The photometric period of V1974 Cygni (Nova Cygni 1992)

DeYoung¹,

Schmidt²

1994

ApJ

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“…Higher temperature emission detected in some nova outbursts (e.g. QU Vul, Taylor et al 1987; V1974 Cyg, Pavelin et al 1993) suggests that, at least for some novae, there is shocked material within the ejected shell.…”

Section: Introductionmentioning

confidence: 96%

V723 Cas (Nova Cassiopeiae 1995): MERLIN observations from 1996 to 2001

Heywood

O’Brien

Eyres

et al. 2005

Monthly Notices of the Royal Astronomical Society

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MERLIN observations of the unusually slow nova V723 Cas are presented. Nine epochs of 6-cm data between 1996 and 2001 are mapped, showing the initial expansion and brightening of the radio remnant, the development of structure and the final decline. A radio light curve is presented and fitted by the standard Hubble flow model for radio emission from novae in order to determine the values of various physical parameters for the shell. The model is consistent with the overall development of the radio emission. Assuming a distance of 2.39 (+/-0.38) kpc and a shell temperature of 17000 K, the model yields values for expansion velocity of 414 +/- 0.1 km s^-1 and shell mass of 1.13 +/- 0.04 * 10^-4 Msolar. These values are consistent with those derived from other observations although the ejected masses are rather higher than theoretical predictions. The structure of the shell is resolved by MERLIN and shows that the assumption of spherical symmetry in the standard model is unlikely to be correct.Comment: 6 pages, 6 figure

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Radio observations of the classical nova Cygni 92 eighty days after outburst

Cited by 45 publications

References 3 publications

The 2011 Outburst of Recurrent Nova T Pyx: Radio Observations Reveal the Ejecta Mass and Hint at Complex Mass Loss

The 2011 Outburst of Recurrent Nova T Pyx: Radio Observations Reveal the Ejecta Mass and Hint at Complex Mass Loss

The photometric period of V1974 Cygni (Nova Cygni 1992)

V723 Cas (Nova Cassiopeiae 1995): MERLIN observations from 1996 to 2001

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