8-13 micron spectrophotometry of planetary nebulae

Aitken, D. K.; Roche, P. F.; Spenser, P. M.; Jones, B.

doi:10.1086/157455

Cited by 69 publications

(40 citation statements)

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“…Superimposed on this continuum are dust features attributed to silicate dust particles (e.g. Aitken et al 1979;Waters et al 1998;Cohen et al 1999) or carbon-based dust particles (e.g. Gillett et al 1973;Waters et al 1998;Cohen et al 1999;Szczerba et al 2001).…”

Section: Introductionmentioning

confidence: 99%

The temperature structure of dusty planetary nebulae

Stasińska¹,

Szczerba²

2001

A&A

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Abstract.We have analyzed the effects of photoelectric heating by dust grains in photoionization models of planetary nebulae. We have shown that this process is particularly important if planetary nebulae contain a population of small grains. The presence of such grains would solve a number of problems that have found no satisfactory solution so far: i) the thermal energy deficit in some objects inferred from tailored photoionization modelling; ii) the large negative temperature gradients inferred directly from spatially resolved observations and indirectly from integrated spectra in some planetary nebulae; iii) the fact that the temperatures derived from the Balmer jump are smaller than those derived from [O iii] λ4363/5007; iv) the fact that the observed intensities of [O i] λ6300 are often larger than predicted by photoionization models. In the presence of moderate density inhomogeneities, such as those inferred from high resolution images of planetary nebulae, photoelectric heating would boost the temperature of the tenuous component, which would then better confine the clumps. The temperature structure of such dusty and filamentary nebulae would solve the long-standing problem of temperature fluctuations posed by Peimbert (1967).

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Section: Introductionmentioning

confidence: 99%

The temperature structure of dusty planetary nebulae

Stasińska¹,

Szczerba²

2001

A&A

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“…The fact that the characteristics of the infrared excess of the object suggest emission by silicate grains (cf. Aitken et al 1979;Scott 1983) and the fact that RY Sct is an IRAS source further support this possibility. An additional argument in favor of this hypothesis is provided by Kwok 's (1990) "infrared sequence in the late stages of stellar evolution".…”

Section: The A4 Absorption System and The Distance To Ry Sctmentioning

confidence: 88%

A Spectrographic Study of the Interacting Eclipsing Binary RY Scuti: An Episode in the Rapid Mass Loss Stage or a Protoplanetary Nebula ?

Sahade¹,

West²,

Skul'Skij³

1992

Evolutionary Processes in Interacting Binary Stars

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RESUMENRY Scuti, la binaria de eclipse de 11 días de período, caracterizada, en su espectro, por presentar líneas de [Fe III], ha sido reinvestigada en base a material espectrográfico obtenido en Chile, en el Observatorio Europeo Austral y en el Observatorio Interamericano de Cerro Tololo, que cubre las regiones 3400-5150Å y 5700-6700Å. Fueron también analizadas observaciones en el ultravioleta obtenidas con el satélite IUE. El espectro de RY Sct es muy complejo y peculiar, y está caracterizado por varios conjuntos de líneas de emisión y de absorción. Entre las emisiones, aparece un grupo de líneas que son características de las nebulosas planetarias. El sistema está formado por una componente B0V y una compañera que parece rodeada por una envoltura opaca que emite en He II λ4686. En la envoltura circumbinaria podemos distinguir: (a) una región de radiación diluida animada de una velocidad de ∼ −178 km s −1 ; (b) regiones donde se originan las líneas de resonancia de Si IV y C IV en el ultravioleta, con velocidades de −1200 y −600 km s −1 ; (c) regiones que dan origen al "espectro nebular" y sugieren la existencia de una triple nebulosidad que rodea al sistema y está caracterizada por un valor de N e probablemente mayor que 10 4 cm −3 , un valor de T e ∼ 15-20,000 K y velocidades de −18, +9 y +48 km s −1 , respectivamente. ABSTRACT RY Scuti, the 11-day [Fe III] eclipsing binary, has been reinvestigated on the basis of spectrographic material obtained in Chile at the European Southern Observatory, La Silla, and at the Cerro Tololo Interamerican Observatory, covering the spectral regions 3400-5150Å and 5700-6700Å. Ultraviolet IUE observations were also analyzed. The spectrum of RY Sct is very complex and peculiar, being characterized by several sets of emission as well as absorption features. Among the emission features, there is a set of lines that are characteristic of planetary nebulae. The system is found to be formed by a B0V component and a companion that appears to be surrounded by an opaque envelope that emits in He II λ4686. In the circumbinary envelope we can distinguish: (a) a region of diluted radiation that suggests a velocity of ∼ −178 km s −1 ; (b) regions of formation of the resonance lines of Si IV and C IV in the IUE UV, characterized by velocities of −1200 and −600 km s −1 ; (c) regions that give rise to the "nebular spectrum" and suggest that there is a triple nebulosity surrounding the system with N e probably larger than 10 4 cm −3 , T e ∼ 15-20,000 K and velocities of −18, +9 and +48 km s −1 , respectively.

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“…These include amorphous silicates (Trapezium emissivity [10]), crystalline silicates (aerosol forsterite and enstatite [11]), amorphous and annealed SiO 2 [12], and SiC (carbon star emissivity [13]). The fitting function can be expressed as F λ ∝ B λ (T ) × e −α , where B λ (T ) is the Planck black-body function at temperature T , α = ∑ k i=1 τ i is the total optical depth of k absorption components and τ i is the optical depth of each component (i.e., all absorptive).…”

Section: Model Fittingmentioning

confidence: 99%

Dust mineralogy in the circumstellar envelope of SVS13

Fujiyoshi¹,

Wright²,

Moore³

2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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It is of great interest to study the mineralogy of circumstellar dust around young stars as it represents the original constituents of planetesimals, hence of the rocky planets like our own Earth. To this end, we have obtained an N-band (8−13 µm) spectrum of a pre-main-sequence star SVS13, using the facility mid-infrared imaging spectrometer COMICS on the Japanese 8.2-m Subaru Telescope atop the summit of Mauna Kea, Hawaii. We have fitted various emissivities/absorption coefficients of dust species to the spectrum to examine dust mineralogy in the circumstellar envelope of this remarkable young star. In this presentation, we outline the modelling and highlight some of our findings.

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8-13 micron spectrophotometry of planetary nebulae

Cited by 69 publications

References 0 publications

The temperature structure of dusty planetary nebulae

The temperature structure of dusty planetary nebulae

A Spectrographic Study of the Interacting Eclipsing Binary RY Scuti: An Episode in the Rapid Mass Loss Stage or a Protoplanetary Nebula ?

Dust mineralogy in the circumstellar envelope of SVS13

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