The phenomenon of osmosis in permeable membranes

Dickel, G.

doi:10.1016/s0021-9673(01)85424-8

Cited by 10 publications

(17 citation statements)

References 6 publications

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“…originate from neutral hydrogen associated with molecular concentrations and absorbing dust in an expanding shell (Dickel 1974). Additional absorption is present at −43.0 and −31.6 km s −1 in Carina S and at +2.8 km s −1 in Carina N, which may be similar to the −1.7 kms −1 feature in ηCarinae (given the similar shift of the main absorption feature).…”

Section: The Carbon Isotope Ratio and The Question Of C + In The Homumentioning

confidence: 68%

η Carinae's Dusty Homunculus Nebula from Near-infrared to Submillimeter Wavelengths: Mass, Composition, and Evidence for Fading Opacity

Morris

Gull

Hillier

et al. 2017

ApJ

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Infrared observations of the dusty, massive Homunculus Nebula around the luminous blue variable η Carinae are crucial to characterize the mass-loss history and help constrain the mechanisms leading to the great eruption. We present the 2.4-670 μm spectral energy distribution, constructed from legacy Infrared Space Observatory observations and new spectroscopy obtained with the Herschel Space Observatory. Using radiative transfer modeling, we find that the two best-fit dust models yield compositions that are consistent with CNO-processed material, with iron, pyroxene and other metal-rich silicates, corundum, and magnesium-iron sulfide in common. Spherical corundum grains are supported by the good match to a narrow 20.2 μm feature. Our preferred model contains nitrides AlN and Si 3 N 4 in low abundances. Dust masses range from 0.25 to 0.44tot in both cases, due to an expected high Fe gas-to-dust ratio. The bulk of dust is within a ´ 5 7 central region. An additional compact feature is detected at 390 μm. We obtain L IR = 2.96×10 6  L , a 25% decline from an average of mid-IR photometric levels observed in 1971-1977. This indicates a reduction in circumstellar extinction in conjunction with an increase in visual brightness, allowing 25%-40% of optical and UV radiation to escape from the central source. We also present an analysis of 12 CO and 13 CO J=5-4 through 9-8 lines, showing that the abundances are consistent with expectations for CNO-processed material. The [ 12 C II] line is detected in absorption, which we suspect originates in foreground material at very low excitation temperatures.

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Section: The Carbon Isotope Ratio and The Question Of C + In The Homumentioning

confidence: 68%

η Carinae's Dusty Homunculus Nebula from Near-infrared to Submillimeter Wavelengths: Mass, Composition, and Evidence for Fading Opacity

Morris

Gull

Hillier

et al. 2017

ApJ

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“…Far-infrared emission associated with the dust lane has also been observed (Harvey et al 1979;Ghosh et al 1988). The velocity structure is explained by a model of molecular gas surrounding the ionized gas and expanding at about 7 km s −1 from a point 15 southwest of η Car (Dickel 1974). Optical observations show strong line splitting near Car II, suggesting that the ionized gas is expanding at 25 km s −1 (Deharveng & Maucherat 1975).…”

Section: Introductionmentioning

confidence: 84%

Detection of highly-ionized diffuse gas in the Galactic plane

Mizutani

Onaka

Shibai

2002

A&A

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lines and two distinct components were seen in the electron density map. One is a component with a density of 100-350 cm −3 , which encloses two H ii regions, Car I and Car II. The other is an extended diffuse component, in which the ratio of the [O iii] lines is nearly at the low electron density limit (ne < 100 cm −3 ). The observed [N iii]/[O iii] line intensity ratio also supports low electron density of the extended gas component. The diffuse component was detected in the entire observed region, which corresponds to ∼30 pc at the distance of the Carina nebula. The present LWS observations of the ionic lines indicate the existence of highly-ionized diffuse gas of low electron density extending around the Carina nebula.

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“…H 2 CO and OH absorption measurements identified two optical depth maxima which were located towards these lanes (Gardner, Dickel & Whiteoak 1970;Dickel & Wall 1974). Extended far-IR emission is confined there also (Harvey, Hoffmann & Campbell 1979;Ghosh et al 1988).…”

Section: Introductionmentioning

confidence: 95%

“…The dark lanes consist of molecular gas and dust that are associated with the nebula (Dickel 1974). H 2 CO and OH absorption measurements identified two optical depth maxima which were located towards these lanes (Gardner, Dickel & Whiteoak 1970;Dickel & Wall 1974).…”

Section: Introductionmentioning

confidence: 99%

An Investigation of the Molecular Clouds of the Carina HII Region/Molecular Cloud Complex—First Results

Brooks¹,

Whiteoak²,

Storey³

1998

Publ. – Astron. Soc. Aust

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Abstract:The Carina Nebula is an extremely bright southern H II region embedded in a giant molecular cloud and contains some of the most massive stars known in our Galaxy. We are undertaking a multi-wavelength study of the Carina Nebula in order to examine the detailed kinematics and distribution of the molecular and ionised gas, and to look for further evidence of ongoing star formation. Here we present the results of the initial molecular cloud observations which were made by observing the 12 CO(1-0) emission with the Mopra antenna. The observations reveal the clumpy morphology of the molecular gas, and allow us to identify many interesting regions for follow-up observations.

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The phenomenon of osmosis in permeable membranes

Cited by 10 publications

References 6 publications

η Carinae's Dusty Homunculus Nebula from Near-infrared to Submillimeter Wavelengths: Mass, Composition, and Evidence for Fading Opacity

η Carinae's Dusty Homunculus Nebula from Near-infrared to Submillimeter Wavelengths: Mass, Composition, and Evidence for Fading Opacity

Detection of highly-ionized diffuse gas in the Galactic plane

An Investigation of the Molecular Clouds of the Carina HII Region/Molecular Cloud Complex—First Results

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