GK Per (Nova Persei 1901): HST Imagery and Spectroscopy of the Ejecta, and First Spectrum of the Jet-Like Feature
arXiv:1204.3078 · doi:10.1088/0004-6256/143/6/143
Abstract
We have imaged the ejecta of GK Persei (Nova Persei 1901 A.D.) with the Hubble Space Telescope (HST), revealing hundreds of cometary-like structures. One or both ends of the structures often show a brightness enhancement relative to the structures' middle sections, but there is no simple regularity to their morphologies (in contrast with the Helix nebula). Some of the structures' morphologies suggest the presence of slow-moving or stationary material with which the ejecta is colliding, while others suggest shaping from a wind emanating from GK Per itself. A detailed expansion map of the nova's ejecta was created by comparing HST images taken in successive years. WFPC2 narrowband images and STIS spectra demonstrate that the physical conditions in the ejecta vary strongly on spatial scales much smaller than those of the ejecta. Directly measuring accurate densities and compositions, and hence masses of this and other nova shells, will demand data at least as resolved spatially as those presented here. The filling factor the ejecta is < 1%, and the nova ejecta mass must be less than $10^{-4} \Msun$. A few of the nebulosities vary in brightness by up to a factor of two on timescales of one year. Finally, we present the deepest images yet obtained of a jet-like feature outside the main body of GK Per nebulosity, and the first spectrum of that feature. Dominated by strong, narrow emission lines of [NII], [OII], [OIII], and [SII], this feature is probably a shock due to ejected material running into stationary ISM, slowly moving ejecta from a previous nova episode, or circum-binary matter present before 1901. An upper limit to the mass of the jet is of order a few times $10^{-6} \Msun$. The jet might be an important, or even dominant mass sink from the binary system. The jet's faintness suggests that similar features could easily have been missed in other cataclysmic binaries.
43 pages, 17 figures
Cited by in corpus (23)
- The Hα surface brightness - radius relation: a robust statistical distance indicator for planetary nebulae
- The Distances to Novae As Seen By Gaia
- A catalogue of cataclysmic variables from 20 years of the Sloan Digital Sky Survey with new classifications, periods, trends and oddities
- Identifying and Quantifying Recurrent Novae Masquerading as Classical Novae
- AT Cnc: A Second Dwarf Nova with a Classical Nova Shell
- The 2011 Outburst of Recurrent Nova T Pyx: Radio Observations Reveal the Ejecta Mass and Hint at Complex Mass Loss
- The Radio Light Curve of the Gamma-Ray Nova in V407 Cyg: Thermal Emission from the Ionized Symbiotic Envelope, Devoured from Within by the Nova Blast
- Discovery of an eclipsing dwarf nova in the ancient nova shell Te 11
- A three-dimensional view of the remnant of Nova Persei 1901 (GK Per)
- Angular Expansion of Nova Shells
- Multi-mission observations of the old nova GK Per during the 2015 outburst
- Precise Measures of Orbital Period, Before and After Nova Eruption for QZ Aurigae
- X-ray Fading and Expansion in the "Miniature Supernova Remnant" of GK Persei
- Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE
- Introducing the Condor Array Telescope: IV. A possible nova super-remnant surrounding the putative recurrent nova KT Eridani
- A multiwavelength light curve analysis of the classical nova YZ Ret: An extension of the universal decline law to the nebular phase
- Radio Frequency Models of Novae in eruption. I. The Free-Free Process in Bipolar Morphologies
- Extended X-ray emission from the classic nova DQ Her -- On the possible presence of a magnetized jet
- A search for cool molecular gas in GK Persei and other classical novae
- The H surface brightness radius plane as a diagnostic tool for photoionized nebulae
- V5856 Sagittarii/2016: Broad Multi-Epoch Spectral Coverage of a Sustained High Luminosity Nova
- Observations and Analysis of the GK Persei Nova Shell and its "Jet-like" Feature
- The Recurrent Nova U Scorpii from the 2010.1 to 2022.4 Eruptions; the Missed Eruption of 2016.78 +- 0.10 and the Critical Complex Period Changes