Flaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a)

Aydi, E.; Chomiuk, Laura; Strader, Jay; Swihart, Samuel J.; Bahramian, A.; Harvey, E. J.; Britt, C. T.; Buckley, D. A. H.; Chen, Ping; Dage, Kristen C.; Darnley, M. J.; Dong, Subo; Hambsch, F. J.; Holoien, Tw-S; Kochanek, C. S.; Kuin, N. P. M.; Li, K. L.; Monard, L. A. G.; Mukai, K.; Page, K. L.; Prieto, J. L.; Richardson, Noel D.; Shappee, B. J.; Shishkovsky, Laura; Sokolovsky, K. V.; Stanek, K. Z.; Thompson, Tom

doi:10.48550/arxiv.1903.09232

Cited by 8 publications

(16 citation statements)

References 74 publications

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“…We also make use of publicly available medium-and high-resolution spectra from the Astronomical Ring for Access to Spectroscopy (ARAS 2 ; Teyssier 2019). For nova ASASSN-17pf, we use data from Aydi et al (2019). These data were obtained using the Magellan Inamori Kyocera Echelle (MIKE) spectrograph mounted on the Magellan Clay telescope (Bernstein et al 2003;Shectman & Johns 2003) and the Echelle Spectrograph mounted on the 2.5 m Irénée Du Pont Telescope 3 .…”

Section: Sample Selectionmentioning

confidence: 99%

“…Unfortunately, there are essentially no theoretical studies that consider all of these potential mass loss mechanisms and model them selfconsistently, so it remains difficult to predict which mechanism will dominate and under which conditions. Meanwhile, observations suggest that multiple mechanisms may be relevant, even within an individual system (e.g., Friedjung 1987;Strope et al 2010;Chomiuk et al 2014), and multiple ejections may occur over a single eruption (e.g., Pejcha 2009;Aydi et al 2019Aydi et al , 2020.…”

Section: Introductionmentioning

confidence: 99%

“…Observations obtained during the eruption itself-which can track changes in mass ejection as they occur-are needed. High-resolution optical spectroscopy during the first days of the eruption can track the velocity (and to some extent, the morphology) of the ejecta, and can therefore be used to constrain ejection scenarios in novae (e.g., McLaughlin 1945McLaughlin , 1947Payne-Gaposchkin 1957;Friedjung 1987;Williams & Mason 2010;Arai et al 2016;Aydi et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Early spectral evolution of classical novae: consistent evidence for multiple distinct outflows

Aydi,

Chomiuk,

Izzo

et al. 2020

Preprint

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The physical mechanism driving mass ejection during a nova eruption is still poorly understood. Possibilities include ejection in a single ballistic event, a common envelope interaction, a continuous wind, or some combination of these processes. Here we present a study of 12 Galactic novae, for which we have pre-maximum high-resolution spectroscopy. All 12 novae show the same spectral evolution. Before optical peak, they show a slow P Cygni component. After peak a fast component quickly arises, while the slow absorption remains superimposed on top of it, implying the presence of at least two physically distinct flows. For novae with high-cadence monitoring, a third, intermediate-velocity component is also observed.These observations are consistent with a scenario where the slow component is associated with the initial ejection of the accreted material and the fast component with a radiation-driven wind from the white dwarf. When these flows interact, the slow flow is swept up by the fast flow, producing the intermediate component. These colliding flows may produce the γ-ray emission observed in some novae. Our spectra also show that the transient heavy element absorption lines seen in some novae have the same velocity structure and evolution as the other lines in the spectrum, implying an association with the nova ejecta rather than a pre-existing circumbinary reservoir of gas or material ablated from the secondary. While this basic scenario appears to qualitatively reproduce multi-wavelength observations of classical novae, substantial theoretical and observational work is still needed to untangle the rich diversity of nova properties.

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Section: Sample Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Early spectral evolution of classical novae: consistent evidence for multiple distinct outflows

Aydi,

Chomiuk,

Izzo

et al. 2020

Preprint

Self Cite

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“…Local maxima ("flares") are observed in classical nova light curves on timescales ranging from hours to weeks (e.g. Strope et al 2010;Walter et al 2012;Henze et al 2018;Aydi et al 2019). To generate collisions on approximately this timescale, we impose transitions between the slow to the fast mode on a characteristic time interval δt ≈ hours−days and with delays between the transitions of a day to a week.…”

Section: Description Of Numerical Modelmentioning

confidence: 99%

“…The photosphere appears to temporarily expand during flares (e.g. Tanaka et al 2011a;Aydi et al 2019), behavior often accompanied by the appearance of new absorption line systems (e.g. Jack et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Internal shocks from variable outflows in classical novae

Steinberg

Metzger

2019

Monthly Notices of the Royal Astronomical Society

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We present one-dimensional hydrodynamical simulations including radiative losses, of internal shocks in the outflows from classical novae, to explore the role of shocks in powering multi-wavelength emission from radio to gamma-ray wavelengths. Observations support a picture in which the initial phases of some novae generate a slow, equatorially-focused outflow (directly from the outer Lagrange point, or from a circumbinary disk), which then transitions to, or is overtaken by, a faster more isotropic outflow from the white dwarf which collides and shocks the slower flow, powering gamma-ray and optical emission through reprocessing by the ejecta. However, the common occurence of multiple peaks in nova light curves suggests that the outflow's acceleration need not be monotonic, but instead can involve successive transitions between "fast" and "slow" modes. Such a time-fluctuating outflow velocity naturally can reproduce several observed properties of nova, such as correlated gamma-ray and optical flares, expansion of the photosphere coincident with (though lagging slightly) the peak flare luminosity, and complex time-evolution of spectral lines (including accelerating, decelerating, and merging velocity components). While the shocks are still deeply embedded during the gamma-ray emission, the onset of ∼ keV X-ray and ∼ 10 GHz radio synchrotron emission is typically delayed until the forward shock of the outermost monolithic shell (created by merger of multiple internal shock-generated shells) reaches a sufficiently low column through the dense external medium generated by the earliest phase of the outburst.

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Radio light curves and imaging of the helium nova V445 Puppis reveal seven years of synchrotron emission

Nyamai

Chomiuk

Ribeiro

et al. 2020

Monthly Notices of the Royal Astronomical Society

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V445 Puppis is the only helium nova observed to date; its eruption in late 2000 showed high velocities up to 8500 km s−1, and a remarkable bipolar morphology cinched by an equatorial dust disc. Here we present multi-frequency radio observations of V445 Pup obtained with the Very Large Array (VLA) spanning 1.5–43.3 GHz, and between 2001 January and 2008 March (days ∼89–2700 after eruption). The radio light curve is dominated by synchrotron emission over these seven years, and shows four distinct radio flares. Resolved radio images obtained in the VLA’s A configuration show that the synchrotron emission hugs the equatorial disc, and comparisons to near-IR images of the nova clearly demonstrate that it is the densest ejecta—not the fastest ejecta—that are the sites of the synchrotron emission in V445 Pup. The data are consistent with a model where the synchrotron emission is produced by a wind from the white dwarf impacting the dense equatorial disc, resulting in shocks and particle acceleration. The individual synchrotron flares may be associated with density enhancements in the equatorial disc and/or velocity variations in the wind from the white dwarf. This overall scenario is similar to a common picture of shock production in hydrogen-rich classical novae, but V445 Pup is remarkable in that these shocks persist for almost a decade, much longer than the weeks or months for which shocks are typically observed in classical novae.

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Flaring, Dust Formation, And Shocks In The Very Slow Nova ASASSN-17pf (LMCN 2017-11a)

Cited by 8 publications

References 74 publications

Early spectral evolution of classical novae: consistent evidence for multiple distinct outflows

Early spectral evolution of classical novae: consistent evidence for multiple distinct outflows

Internal shocks from variable outflows in classical novae

Radio light curves and imaging of the helium nova V445 Puppis reveal seven years of synchrotron emission

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