A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Finzell, Thomas; Chomiuk, Laura; Metzger, Brian D.; Walter, Frederick M.; Linford, Justin D.; Mukai, K.; Nelson, Thomas; Weston, Jennifer; Zheng, Yong; Sokoloski, J. L.; Mioduszewski, Amy J.; Rupen, M. P.; Dong, Subo; Starrfield, S.; Cheung, C. C.; Woodward, C. E.; Taylor, G. B.; Bohlsen, T.; Buil, C.; Prieto, J. L.; Wagner, R. M.; Bensby, T.; Bond, I. A.; Sumi, T.; Bennett, D. P.; Abe, F.; Koshimoto, Naoki; Suzuki, D.; Tristram, P. J.; Christie, Grant; Natusch, T.; McCormick, J.; Yee, Jennifer C.; Gould, A.

doi:10.3847/1538-4357/aaa12a

Cited by 40 publications

(41 citation statements)

References 110 publications

(232 reference statements)

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“…The same spectroscopic signature was observed in the recent dust forming CO nova V1324 Sco (Finzell et al 2018). Although the line profiles presented in that paper cover only the period before the main event, that part of the expansion when the ejecta transitioned to optically thin in the Fe-curtain, one Balmer line profile taken 800 days after the deep minimum shows precisely the same signature as we have shown here for late spectra.…”

Section: Dust Signatures In Other Novaesupporting

confidence: 83%

Spectroscopic diagnostics of dust formation and evolution in classical nova ejecta

Shore

Kuin

Mason

et al. 2018

A&A

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A fraction of classical novae form dust during the early stages of their outbursts. The classical CO nova V5668 Sgr (Nova Sgr. 2015b) underwent a deep photometric minimum about 100 days after outburst that was covered across the spectrum. A similar event was observed for an earlier CO nova, V705 Cas (Nova Cas 1993) and a less optically significant event for the more recent CO nova V339 Del (Nova Del 2013). This study provides a "compare and contrast" of these events to better understand the very dynamical event of dust formation. We show the effect of dust formation on multiwavelength high resolution line profiles in the interval 1200Å -9200Å using a biconical ballistic structure that has been applied in our previous studies of the ejecta. We find that both V5668 Sgr and V339 Del can be modeled using a grey opacity for the dust, indicating fairly large grains ( 0.1µ) and that the persistent asymmetries of the line profiles in late time spectra, up to 650 days after the event for V5668 Sgr and 866 days for V339 Del, point to the survival of the dust well into the transparent, nebular stage of the ejecta evolution. This is a general method for assessing the properties of dust forming novae well after the infrared is completely transparent in the ejecta.

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Section: Dust Signatures In Other Novaesupporting

confidence: 83%

Spectroscopic diagnostics of dust formation and evolution in classical nova ejecta

Shore

Kuin

Mason

et al. 2018

A&A

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“…The equatorial wind ejecta is opaque in the continuum at this phase leading to spectra that, despite the somewhat unusual geometry, could well appear consistent with the usual optically-thick early stage of the nova outburst. L2 spiral shocks powering early-time optical emission from novae would be consistent with observations of periodicities at the orbital period in the early-time light curves of some novae [30][31][32] .…”

supporting

confidence: 85%

“…We adopted the linear MMRD distance of d = 4.2 kpc as a reference distance in our analysis but caution that the uncertainties in the distance do not include systematic uncertainties in the MMRD. For example, Kasliwal et al 32 found that some novae with t 2 ∼ 10 days (the observed value for ASASSN-16ma) were up to 2 mag fainter than predicted by the MMRD, which would imply a distance of only 1.7 kpc. At this short distance the inferred luminosity could be consistent with the Eddington luminosity, depending on the mass of the white dwarf.…”

mentioning

confidence: 93%

A nova outburst powered by shocks

et al. 2017

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Classical novae are runaway thermonuclear burning events on the surfaces of accreting white dwarfs in close binary star systems, sometimes appearing as new naked-eye sources in the night sky 1 . The standard model of novae predicts that their optical luminosity derives from energy released near the hot white dwarf which is reprocessed through the ejected material [2][3][4][5] . Recent studies with the Fermi Large Area Telescope have shown that many classical novae are accompanied by gigaelectronvolt γ-ray emission 6, 7 . This emission likely originates from strong shocks, providing new insights into the properties of nova outflows and allowing them to be used as laboratories to study the unknown efficiency of particle acceleration in shocks. Here we report γ-ray and optical observations of the Milky Way nova ASASSN-16ma, which is among the brightest novae ever detected in γ-rays. The γ-ray and optical light curves show a remarkable correlation, implying that the majority of the optical light comes from reprocessed emission from shocks rather than the white dwarf 8 . The ratio of γ-ray to optical flux in ASASSN-16ma directly constrains the acceleration efficiency of non-thermal particles to be ∼ 0.005, favouring hadronic models for the γ-ray emission 9 .The need to accelerate particles up to energies exceeding 100 gigaelectronvolts provides compelling evidence for magnetic field amplification in the shocks.ASASSN-16ma (a.k.a. PNV J18205200−2822100, Nova Sgr 2016d, and V5856 Sgr) is an optical transient source in the constellation Sagittarius, discovered by the All Sky Automated Survey for SuperNovae (ASAS-SN 10 ), on 25.02 October 2016 UT 11 (a corresponding Modified Julian Day of MJD 57686.02) and identified as a normal classical nova with optical spectroscopy 12, 13 .The optical light curve of the nova after its discovery shows three distinct phases (Figure 1). In Phase I, the nova slowly rose to m V ∼ 8 mag over two weeks. It then showed a rapid brightening by a factor of ∼ 10 over just two days (Phase II), reaching a naked-eye peak visual magnitude of 5.4 (MJD 57700). This was followed by a relatively stable decline lasting for several weeks (Phase III; see Figure 1 and Methods).Immediately following the optical peak, our Fermi target-of-opportunity (ToO) observation detected strong γ-ray emission from the nova with a very high photon flux of F ph,γ ≈ 2 10 −6 ph cm −2 s −1 (Methods). The γ-ray emission faded rapidly over the next nine days, with only marginal γ-ray detections in the following week. This is among the fastest-evolving γ-ray light curves seen to date from a nova. The optical and γ-ray light curves are tightly correlated, declining at the same rate and showing a simultaneous dip in the emission around MJD 57705 (Figure 1). The ratio of the γ-ray to optical luminosity (∼ 0.002) remains constant while the γ-rays are detectable (Figure 1; see also Supplementary Information, SI hereafter).The clear correlation between the γ-ray and optical light in ASASSN-16ma leads us to reconsider the standard mod...

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“…Another source studied by Rupen's team, V1723 Aql, showed an unexpectedly rapid turn-on in the radio, an anomalous spectral index (α ∝ ν 1.3 ), a double-peaked radio light curve, and T B > 10 6 K (Weston et al 2016b). A double-peaked radio light curve was also seen in V1324 Sco (Finzell et al 2018).…”

Section: Cataclysmic Variables (Cvs)mentioning

confidence: 76%

Radio Stars: From kHz to THz

Matthews¹

2018

PASP

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Advances in technology and instrumentation have now opened up virtually the entire radio spectrum to the study of stars. An international workshop Radio Stars: from kHz to THz was held at the Massachusetts Institute of Technology Haystack Observatory on 2017 November 1-3 to enable the discussion of progress in solar and stellar astrophysics enabled by radio wavelength observations. Topics covered included the Sun as a radio star, radio emission from hot and cool stars (from the pre-to post-main-sequence), ultracool dwarfs, stellar activity, stellar winds and mass loss, planetary nebulae, cataclysmic variables, classical novae, and the role of radio stars in understanding the Milky Way. This article summarizes meeting highlights along with some contextual background information.

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A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Cited by 40 publications

References 110 publications

Spectroscopic diagnostics of dust formation and evolution in classical nova ejecta

Spectroscopic diagnostics of dust formation and evolution in classical nova ejecta

A nova outburst powered by shocks

Radio Stars: From kHz to THz

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