On linear light polarization of novae: dust envelopes

Kučinskas, A.

doi:10.1002/asna.2113110114

Cited by 3 publications

(2 citation statements)

References 26 publications

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“…For ASASSN-17pf the second spectropolarimetric observations were obtained after the recovery from the dust dip. Thus, the polarization might also be due to scattering by the remaining dust grains from the dust formation event (Kucinskas 1990;Gehrz 2008). Another source of LP in novae is the asymmetry of the expanding ejecta (e.g., Bjorkman et al 1994).…”

Section: Polarizationmentioning

confidence: 99%

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

Aydi¹,

Chomiuk²,

Strader³

et al. 2019

Preprint

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We present a detailed study of the 2017 eruption of the classical nova ASASSN-17pf (LMCN 2017-11a), which is located in the Large Magellanic Cloud, including data from AAVSO, ASAS-SN, SALT, SMARTS, SOAR, and the Neil Gehrels Swift Observatory. The optical light-curve is characterized by multiple maxima (flares) on top of a slowly evolving light-curve (with a decline time, t 2 > 100 d). The maxima correlate with the appearance of new absorption line systems in the optical spectra characterized by increasing radial velocities. We suggest that this is evidence of multiple episodes of mass-ejection with increasing expansion velocities. The line profiles in the optical spectra indicate very low expansion velocities (FWHM ∼ 190 km s −1 ), making this nova one of the slowest expanding ever observed, consistent with the slowly evolving light-curve. The evolution of the colors and spectral energy distribution show evidence of decreasing temperatures and increasing effective radii for the pseudo-photosphere during each maximum. The optical and infrared light-curves are consistent with dust formation 125 days post-discovery. We speculate that

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Section: Polarizationmentioning

confidence: 99%

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

Aydi¹,

Chomiuk²,

Strader³

et al. 2019

Preprint

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“…Deep imaging and spectroscopic observations of old nova remnants have revealed that many of them have asymmetric structures, such as prolate shells including rings and blobs (e.g., Slavin, O'Brien, & Dunlop 1995;Paresce et al 1995;Gill & O'Brien 2000;Krautter et al 2002;Harman & O'Brien 2003). In addition, polarimetry has revealed that the asymmetric geometry was already present at the outburst phase for many novae (Eggen, Mathewson, & Serkowski 1967;Zellner & Morrison 1971;Piirola & Korhonen 1979;Bergner et al 1988;Kikuchi, Kondo, & Mikami 1988;Kučinskas 1990;Bjorkman et al 1994;El'kin 1995;Okazaki et al 1996;Johnson et al 1997;Kawabata et al 2001;Evans et al 2002;Wisniewski et al 2003;Desidera et al 2004). However, despite the accumulation of observational facts, it is still not clear what gives rise to departures from spherical symmetry in nova ejecta.…”

Section: Introductionmentioning

confidence: 99%

Low- and Medium-Dispersion Spectropolarimetry of Nova V475 Scuti (Nova Scuti 2003): Discovery of an Asymmetric High-Velocity Wind in a Moderately Fast Nova

et al. 2006

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We present low-resolution (R ∼ 90) and medium-resolution (R ∼ 2500) spectropolarimetry of Nova V475 Sct with the HBS instrument, mounted on the 0.91-m telescope at the Okayama Astrophysical Observatory, and with FOCAS, mounted on the 8.2-m Subaru telescope. We estimated the interstellar polarization toward the nova from the steady continuum polarization components and Hα line emission components. After subtracting the interstellar polarization component from the observations, we found that the Hα emission seen on 2003 October 7 was clearly polarized. In the polarized flux spectrum, the Hα emission had a distinct red wing extending to ∼ +4900 km s −1 and a shoulder around +3500 km s −1 , showing a constant position angle of linear polarization θ * ≃ 155 • ±15 • . This suggests that the nova had an asymmetric outflow with a velocity of v wind ≃ 3500 km s −1 or more, which is six times higher than the expansion velocity of the ionized shell at the same epoch. Such a high-velocity component has not previously been reported for a nova in the 'moderately fast' speed class. Our observations suggest the occurrence of violent mass-loss activity in the nova binary system even during the common-envelope phase. The position angle of the polarization in the Hα wing is in good agreement with that of the continuum polarization found on 2003 September 26 (p * ≃ 0.4-0.6 %), which disappeared within the following 2 d. The uniformity of the PA between the continuum polarization and the wing polarization on October 7 suggests that the axis of the circumstellar asymmetry remained nearly constant during the period of our observations.

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Nova V4444 Sagittarii 1999: Spectropolarimetric Evidence for a Preexisting Circumstellar Dust Cloud

Kawabata

Hirata

Ikeda

et al. 2000

ApJ

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On linear light polarization of novae: dust envelopes

Cited by 3 publications

References 26 publications

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

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

Low- and Medium-Dispersion Spectropolarimetry of Nova V475 Scuti (Nova Scuti 2003): Discovery of an Asymmetric High-Velocity Wind in a Moderately Fast Nova

Nova V4444 Sagittarii 1999: Spectropolarimetric Evidence for a Preexisting Circumstellar Dust Cloud

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