Mid-Infrared Spectroscopic Observations of the Dust-Forming Classical Nova V2676 Oph*

Kawakita, Hideyo; Ootsubo, Takafumi; Arai, Akira; Shinnaka, Yoshiharu; Nagashima, M.

doi:10.3847/1538-3881/153/2/74

Cited by 11 publications

(19 citation statements)

References 36 publications

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“…This observation is not consistent with traditional equilibrium thermodynamic calculations of dust condensation in circumstellar environments that predict formation of carbonaceous grains in Crich stellar envelopes with C/O > 1 and silicate and oxide dust in O-rich envelopes with C/O <1. However, our detection of nanocrystalline silicate and oxide grains inside of a graphite spherule is consistent with astronomical observations over periods of several years in CO nova ejecta that report production of both C-rich (e.g., graphite, SiC and amorphous carbon) and O-rich (e.g., silicates) dust [6][7][8][9][10] .…”

supporting

confidence: 91%

Laboratory evidence for co-condensed oxygen- and carbon-rich meteoritic stardust from nova outbursts

et al. 2019

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Although their parent stars no longer exist, the isotopic and chemical compositions and microstructure of individual stardust grains identified in meteorites provide unique constraints on dust formation and thermodynamical conditions in stellar outflows 1-4. Novae are stellar explosions that take place in the hydrogen-rich envelope accreted onto the surface of a white dwarf in a close binary system 5. The energy released by a suite of nuclear processes operating in the envelope 2 powers a thermonuclear runaway, resulting in the ejection of processed material into the interstellar medium. Spectral fitting of features observed in the infrared spectra of dust-forming novae provided the first evidence of the co-condensation of both carbonaceous and silicate dust in stellar outflows within the 50 to 100 days after explosion 6-11. Here we report the identification of an O-rich inclusion, composed of both silicate and oxide nanoparticles, inside a graphite spherule that originated in the ejecta of a low-mass CO nova 12. This observation provides laboratory evidence of the co-condensation of O-and C-rich dust in nova outbursts, and is consistent with the transport and mixing of materials between chemically distinct clumps within the nova ejecta. Dust in stellar and interstellar environments is traditionally studied using space or ground-based telescopes but the laboratory study of circumstellar (presolar) grains identified in extraterrestrial materials (e.g., meteorites) has opened up a new field in astronomy and astrophysics, providing direct ground-truth information on individual stars. Such presolar grains are nanometer-to micrometer-sized minerals, amorphous grains, or aggregates of them, and can include materials such as nanodiamond, SiC, graphites, oxides, and silicates 1,2. Over the last two decades, about 2000 presolar graphite spherules have been identified and studied exclusively from the acid-resistant residues of the three carbonaceous chondrites: Murchison (CM2), Orgueil (CI1), and Qingzhen (EH3) 13-15. While most presolar graphite spherules originated from lowmetallicity asymptotic-giant-branch stars (∼50%) and core-collapse supernovae (∼25%), the remaining grains are hypothesized to have also originated from other types of stars, e.g., born-again AGB and Jtype stars 14,15. A few presolar graphite grains also have isotopic compositions suggesting possible origins in the ejecta of novae 16. Novae are traditionally classified as neon and non-neon, which reflects the composition of the white dwarf that hosts the explosion, i.e., ONe (O-and Ne-rich) and CO (C-and O-rich), respectively 5. Similarly to other SiC, silicates, and oxides with putative nova origins, these

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supporting

confidence: 91%

Laboratory evidence for co-condensed oxygen- and carbon-rich meteoritic stardust from nova outbursts

et al. 2019

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“…The unidentified-IR (UIR) emission line at 11.4 µm which is sometimes observed in dustforming novae (e.g., V705 Cas [15]), was also detected in V2676 Oph [34]. This emission may be due to free-flying PAH molecules or HAC grains.…”

Section: Dust Formationmentioning

confidence: 87%

“…Direct evidence for the existence of dust grains was obtained by mid-infrared spectroscopic and photometric observations of V2676 Oph, carried out after dust formation, at days t = 452 and 782 [34]. Both amorphous carbon grains and silicate grains were found to exist simultaneously in V2676 Oph (Figure 7).…”

Section: Dust Formationmentioning

confidence: 95%

“…This fact strongly supports the conclusion that V2676 Oph involves a CO WD. Figure 1 of [34]. The black solid lines represent the synthesized spectra at each epoch.…”

Section: Dust Formationmentioning

confidence: 99%

“…The classical nova V2676 Oph is unique in that C 2 , CN, and CO molecules -and larger molecules such as polycyclic aromatic hydrocarbons (PAHs) or hydrogenated amorphous carbon (HAC) -have all been detected in the same nova. In addition, significant dust formation began ∼90 days after the nova explosion [36,51,34,46]. Dust formation is recognized in about ∼20% of classical novae [59] and usually occurs in "CO novae" that involve CO 1 white dwarfs (WDs), whereas dust formation rarely occurs in "ONe novae" involving ONe WDs [20].…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A Review of the Evolution of Classical Nova V2676 Oph: Formation of Molecules and Dust Grains

Kawakita¹,

Arai²

2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

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The Formation of Bimodal Dust Species in Nova Ejecta

Duolikun

Zhu

Wang

et al. 2019

PASP

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The formation of bimodal dust species (namely the silicate and amorphous carbon dust grains coexistent) in a nova eruption is an open problem. According to the nova model simulated by Modules for Experiments in Stellar Astrophysics code, we calculate the formation and growth carbon (C) and forsterite (Mg 2 SiO 4 ) dust grains in nova ejecta for the free-expansion model and the radiative shock model, respectively. In the free-expansion model, the nova ejecta is not an idea environment for dust nucleation. However, it can efficiently produce dust in the radiative shock model. We estimate that every nova can produce C grains with an average mass of about 10 −9 and 10 −8 M ⊙ , and Mg 2 SiO 4 grains with an average mass of about 10 −8 and 10 −7 M ⊙ . Based on the mass of ejected gas, the ratio of dust to gas is about 1%. The C grains form first after several or tens of days of nova eruption. After that, the Mg 2 SiO 4 grains begin to grow in tens of days, which is consistent with observations.

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Mid-Infrared Spectroscopic Observations of the Dust-Forming Classical Nova V2676 Oph*

Cited by 11 publications

References 36 publications

Laboratory evidence for co-condensed oxygen- and carbon-rich meteoritic stardust from nova outbursts

Laboratory evidence for co-condensed oxygen- and carbon-rich meteoritic stardust from nova outbursts

A Review of the Evolution of Classical Nova V2676 Oph: Formation of Molecules and Dust Grains

The Formation of Bimodal Dust Species in Nova Ejecta

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