GK Per (Nova Persei 1901):<i>HUBBLE SPACE TELESCOPE</i>IMAGERY AND SPECTROSCOPY OF THE EJECTA, AND FIRST SPECTRUM OF THE JET-LIKE FEATURE

Shara, Michael M.; Zurek, David; Marco, Orsola De; Mizusawa, Trisha; Williams, Robert E.; Livio, Mario

doi:10.1088/0004-6256/143/6/143

Cited by 39 publications

(41 citation statements)

References 36 publications

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“…However, there are significant differences from the values given by Shafter (1997) and from those, generally higher, found by Weight (1994) and by Ringwald et al (1996) in studies of the optical and IR spectra of cataclysmic variables. For GK Per, and based on the nova galactic coordinates,an estimate of the distance, and the dust prescription of Schlegel et al (1988), Shara et al (2012) derived E(B − V) = 0.32, a value very close to the one derived in this study.…”

Section: The Reddening Correctionsupporting

confidence: 87%

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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Section: The Reddening Correctionsupporting

confidence: 87%

An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

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“…Some deviation from the circular symmetry is, however, visible because the diameter of the nebula in the NE-SW direction is smaller (105 as measured in the 2011 image) than in the NW-SE direction (118 ). As described in detail by Shara et al (2012), the nebula is composed of hundreds of knots and filaments of different sizes and brightnesses. Many of the knots have tails pointing either toward or away from Seaquist et al (1989).…”

Section: Description Of the Nebulamentioning

confidence: 99%

“…Many of the knots have tails pointing either toward or away from Seaquist et al (1989). b Published in Shara et al (2012). c Published in Bode et al (2004).…”

Section: Description Of the Nebulamentioning

confidence: 99%

“…A study of the proper motions in GK Persei remnant knots was recently done by Shara et al (2012) using the 1995 and 1997 HST images listed in Table 1. The proper motions of 938 knots are estimated, but no quantitative comparison with our measurements is possible as Shara et al (2012) did not publish data for individual knots.…”

Section: Comparison With Published Datamentioning

confidence: 99%

“…The proper motions of 938 knots are estimated, but no quantitative comparison with our measurements is possible as Shara et al (2012) did not publish data for individual knots. In spite of the higher resolution of HST, the seven-times-longer baseline of our observations, the large number of measurements (19, which reduce statistical errors), and the accurate knowledge of the astrometric properties of the INT prime-focus camera provide proper-motion measurements that are more accurate by a factor of four (see Figure 8 in Shara et al 2012). Anupama & Prabhu (1993) have measured the motion in the plane of the sky of 20 individual bright knots using two groundbased images obtained on 1984.…”

Section: Comparison With Published Datamentioning

confidence: 99%

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A THREE-DIMENSIONAL VIEW OF THE REMNANT OF NOVA PERSEI 1901 (GK Per)

Liimets

Corradi

Santander-García

et al. 2012

ApJ

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We present a kinematical study of the optical ejecta of GK Per. It is based on proper-motion measurements of 282 knots from ∼20 images spanning 25 years. Doppler shifts are also computed for 217 knots. The combination of proper motions and radial velocities allows a unique three-dimensional view of the ejecta to be obtained. The main results are as follows: (1) the outflow is a thick shell in which knots expand with a significant range of velocities, mostly between 600 and 1000 km s −1 , (2) kinematical ages indicate that knots have suffered only a modest deceleration since their ejection a century ago, (3) no evidence for anisotropy in the expansion rate is found, (4) velocity vectors are generally aligned along the radial direction, but a symmetric pattern of non-radial velocities is also observed at specific directions, and (5) the total Hα+[N ii] flux has been linearly decreasing at a rate of 2.6% per year in the past decade. The eastern nebular side is fading at a slower rate than the western side. Some of the knots were displayed a rapid change of brightness during the 2004-2011 period. Over a longer timescale, a progressive circularization and homogenization of the nebula are taking place; (6) a kinematic distance of 400 ± 30 pc is determined. These results raise some problems with the previous interpretations of the evolution of GK Per. In particular, the idea of a strong interaction of the outflow with the surrounding medium in the southwest quadrant is not supported by our data.

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A search for cool molecular gas in GK Persei and other classical novae

Kamiński

Mazurek

Menten

et al. 2022

A&A

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Detecting molecular line emission from classical nova remnants has the potential to reveal information on the composition of the ejecta, in particular accurate isotopic ratios in the matter processed by a thermonuclear runaway. We conducted searches toward more than 100 classical novae for emission in lines of CO or HCN molecules using single-dish telescopes and interferometric arrays at millimeter and submillimeter wavelengths. The survey demonstrates that classical novae, young or old, are not strong sources of molecular emission at submillimeter or millimeter wavelengths. Additionally, we mapped CO emission around Nova Persei 1901 (GK Per), earlier claimed to be of circumstellar origin. Our measurements indicate that the observed emission is from the interstellar medium. Although no molecular emission at millimeter or submillimeter wavelengths has been found in classical novae, it is still likely that some will be detected with high-sensitivity interferometers such as ALMA.

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GK Per (Nova Persei 1901):HUBBLE SPACE TELESCOPEIMAGERY AND SPECTROSCOPY OF THE EJECTA, AND FIRST SPECTRUM OF THE JET-LIKE FEATURE

Cited by 39 publications

References 36 publications

An archive study of 18 old novae

An archive study of 18 old novae

A THREE-DIMENSIONAL VIEW OF THE REMNANT OF NOVA PERSEI 1901 (GK Per)

A search for cool molecular gas in GK Persei and other classical novae

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