A survey of nova remnants

Duerbeck, H. W.; Seitter, W. C.

doi:10.1007/bf00668127

Cited by 40 publications

(38 citation statements)

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“…One of the main findings from Liimets et al, 2012 was there is no significant deceleration of the knots in the SW quadrant of the nova shell, though it had been long believed that the shell had been experiencing a stronger interaction with circumbinary material in this quadrant Duerbeck et al, 1987. The barrel with polar over-densities structure presented here, as well as the basic bullet crushing time calculation support their finding.…”

Section: Discussion and Questionssupporting

confidence: 70%

Observations and Analysis of the GK Persei Nova Shell and its “Jet-like” Feature

Harvey

Redman

Boumis

et al. 2015

EAS Publications Series

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Abstract. GK Persei (1901, the 'Firework Nebula') is an old but bright nova remnant that offers a chance to probe the physics and kinematics of nova shells. The kinematics in new and archival longslit optical echelle spectra were analysed using the shape software. New imaging from the Aristarchos telescope continues to track the proper motion, extinction and structural evolution of the knots, which have been observed intermittently over several decades. We present for the first time, kinematical constraints on a large faint 'jet' feature, that was previously detected beyond the shell boundary. These observational constraints allow for the generation of models for individual knots, interactions within knot complexes, and the 'jet' feature. Put together, and taking into account dwarf-nova accelerated winds emanating from the central source, these data and models give a deeper insight into the GK Per nova remnant as a whole.

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Section: Discussion and Questionssupporting

confidence: 70%

Observations and Analysis of the GK Persei Nova Shell and its “Jet-like” Feature

Harvey

Redman

Boumis

et al. 2015

EAS Publications Series

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“…T Aur, Q Cyg, DN Gem, CP Lac, DI Lac, DK Lac, GI Mon, V841 Oph), while the λ 4686 line is generally reported in all old novae (see Kraft 1964;Warner 1976;Williams 1983;Duerbeck & Seitter 1987;Ringwald 1996;Bode & Evans 2008b;Bianchini et al 2012), with the only possible exception of DK Lac. This contrasts with an expected line ratio λ 1640/λ 4686 close to 7.0 (Dopita & Sutherland 2003).…”

Section: The Uv Emission Linesmentioning

confidence: 99%

An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

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Aims. We present an overview of the UV spectral properties of old novae as a class. The data and results of this paper, together with data from the outburst phases, will be utilized in a follow-up study to determine statistical properties and to investigate correlations among the physical parameters of the quiescent and eruptive phases. Methods. All the available IUE, HST, and FUSE archive data for 18 old novae were used to derive accurate and homogeneous estimates of the reddening from the 2175 Å extinction bump and to determine the intrinsic spectral energy distribution corresponding to the utilization of both existing extinction curves. We also measured all the emission and absorption lines. Results. We have found good agreement between spectra taken at different epochs and by different instruments, a clear indication of the near constancy of the SED on timescales of several years. With the possible exception of GK Per, the dereddened UV continua are represented well by a single-curve power-law distribution F λ ∝ λ −α , with α in the range 0.32-2.55 for one curve and 0.35-2.88 for the other one. The extrapolation of the various UV power laws to the optical range yields values that are in good agreement with the V magnitudes. We interpret this result as evidence that the SED is dominated by the accretion disk in the UV and optical spectral regions. A detailed study of the emission spectrum has led to measuring and identifying more than one hundred features and to detecting several lines that are rather uncommon in other CVs and whose identification is uncertain.

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“…An eventual circularisation of the shell was proposed in L12. From considerations of the data presented in L12 as well as others, such as Duerbeck & Seitter (1987); Lawrence et al (1995); Tweedy (1995) and Shara et al (2012), the opportunity to explore the structure and kinematics of the GK Per nova shell was undertaken. Knots associated with the shell are expanding almost radially away from the central system and have been followed over the decades; highquality spectroscopy is also available.…”

Section: Introductionmentioning

confidence: 99%

Modelling the structure and kinematics of the Firework nebula: The nature of the GK Persei nova shell and its jet-like feature

Harvey

Redman

Boumis

et al. 2016

A&A

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Aims. The shaping mechanisms of old nova remnants are probes for several important and unexplained processes, such as dust formation and the structure of evolved star nebulae. To gain a more complete understanding of the dynamics of the GK Per (1901) remnant, an examination of symmetry of the nova shell is explored, followed by a kinematical analysis of the previously detected jet-like feature in the context of the surrounding fossil planetary nebula. Methods. Faint-object high-resolution echelle spectroscopic observations and imaging were undertaken covering the knots which comprise the nova shell and the surrounding nebulosity. New imaging from the Aristarchos telescope in Greece and long-slit spectra from the Manchester Echelle Spectrometer instrument at the San Pedro Mártir observatory in Mexico were obtained, supplemented with archival observations from several other optical telescopes. Position-velocity arrays are produced of the shell, and also individual knots, and are then used for morpho-kinematic modelling with the shape code. The overall structure of the old knotty nova shell of GK Per and the planetary nebula in which it is embedded is then analysed. Results. Evidence is found for the interaction of knots with each other and with a wind component, most likely the periodic fast wind emanating from the central binary system. We find that a cylindrical shell with a lower velocity polar structure gives the best model fit to the spectroscopy and imaging. We show in this work that the previously seen jet-like feature is of low velocity. Conclusions. The individual knots have irregular tail shapes; we propose here that they emanate from episodic winds from ongoing dwarf nova outbursts by the central system. The nova shell is cylindrical, not spherical, and the symmetry axis relates to the inclination of the central binary system. Furthermore, the cylinder axis is aligned with the long axis of the bipolar planetary nebula in which it is embedded. Thus, the central binary system is responsible for the bipolarity of the planetary nebula and the cylindrical nova shell. The gradual planetary nebula ejecta versus sudden nova ejecta is the reason for the different degrees of bipolarity. We propose that the 'jet' feature is an illuminated lobe of the fossil planetary nebula that surrounds the nova shell.

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A survey of nova remnants

Cited by 40 publications

References 0 publications

Observations and Analysis of the GK Persei Nova Shell and its “Jet-like” Feature

Observations and Analysis of the GK Persei Nova Shell and its “Jet-like” Feature

An archive study of 18 old novae

Modelling the structure and kinematics of the Firework nebula: The nature of the GK Persei nova shell and its jet-like feature

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