scholarly journals Origin and evolution of the Galactic inventories of interstellar dust and its composition

2020 ◽  
Vol 494 (3) ◽  
pp. 4149-4167
Author(s):  
Anuj Gupta ◽  
Sandeep Sahijpal
Keyword(s):  
Interstellar Dust ◽  
Galactic Centre ◽  
Dust Grains ◽  
Thermodynamical Equilibrium ◽  
Origin And Evolution ◽  
Isotopic Signatures ◽  
Interstellar Dust Grains ◽  
Wide Range ◽  
Dust Mass ◽  
The Galaxy

ABSTRACT Interstellar dust is a significant component of matter in the galaxies. The dust owns its origin and reprocessing in a wide range of astrophysical environments. In order to understand the origin and evolution of the distinct types of interstellar dust grains, we have attempted a comprehensive correlated study of the thermodynamics condensation of dust grains in distinct stellar environments with the Galactic chemical evolution of the Milky Way Galaxy. The Galaxy is evolved in terms of elemental evolution resulting from stellar nucleosynthetic contributions of several generations of stars. Based on the elemental composition of the evolving Galaxy, the relative abundances of the major constituents of interstellar dust are assessed. The major aim is to redistribute the various condensable elements at any epoch during the evolution of the Galaxy into various grain constituents and understand their abundance evolution based on a mass-balance formalism. We also performed thermodynamical equilibrium condensation calculations to understand the stellar origin of various grain constituents that could carry the isotopic signatures of the various stellar nucleosynthetic sources. This is perhaps a novel attempt to estimate the bulk dust mass budget in the evolving Galaxy. The normalized mass of the Galactic dust is predicted to decrease with the increase in distance from the Galactic centre. It increases over time. The supernovae SNe Ia are predicted as the most prominent sources of Fe-dust mass, the supernova SN II+Ib/c produces oxides- and silicate-dust mass, and the AGB stars contribute to carbonaceous dust mass.

scholarly journals Magnesium and silicon in interstellar dust: X-ray overview

2020 ◽  
Vol 641 ◽  
pp. A149
Author(s):  
D. Rogantini ◽  
E. Costantini ◽  
S. T. Zeegers ◽  
M. Mehdipour ◽  
I. Psaradaki ◽  
...  
Keyword(s):  
Cross Sections ◽  
Interstellar Dust ◽  
Galactic Centre ◽  
X Rays ◽  
Dust Grains ◽  
Large Reservoir ◽  
X Ray ◽  
Synchrotron Facility ◽  
The Galaxy ◽  
X Ray Binaries

Context. The dense Galactic environment is a large reservoir of interstellar dust. Therefore, this region represents a perfect laboratory to study the properties of cosmic dust grains. X-rays are the most direct way to detect the interaction of light with dust present in these dense environments. Aims. The interaction between the radiation and the interstellar matter imprints specific absorption features on the X-ray spectrum. We study them with the aim of defining the chemical composition, the crystallinity, and structure of the dust grains that populate the inner regions of the Galaxy. Methods. We investigated the magnesium and the silicon K-edges detected in the Chandra /HETG spectra of eight bright X-ray binaries, distributed in the neighbourhood of the Galactic centre. We modelled the two spectral features using accurate extinction cross-sections of silicates, which we measured at the synchrotron facility Soleil, France. Results. Near the Galactic centre, magnesium and silicon show abundances similar to the solar ones and they are highly depleted from the gas phase (δMg > 0.90 and δSi > 0.96). We find that amorphous olivine with a composition of MgFeSiO4 is the most representative compound along all lines of sight according to our fits. The contribution of Mg-rich silicates and quartz is low (less than 10%). On average we observe a percentage of crystalline dust equal to 11%. For the extragalactic source LMC X-1, we find a preference for forsterite, a magnesium-rich olivine. Along this line of sight we also observe an under-abundance of silicon ASi∕ALMC = 0.5 ± 0.2.

Temperature fluctuations in interstellar dust grains

1979 ◽  
Vol 65 (1) ◽  
pp. 155-166 ◽  
Author(s):  
Per A. Aannestad ◽  
Scott J. Kenyon
Keyword(s):  
Interstellar Dust ◽  
Temperature Fluctuations ◽  
Dust Grains ◽  
Interstellar Dust Grains

scholarly journals DIBs, Interstellar Dust, and Extinction

2013 ◽  
Vol 9 (S297) ◽  
pp. 147-152 ◽  
Author(s):  
G. C. Clayton
Keyword(s):  
Interstellar Medium ◽  
Interstellar Dust ◽  
Dust Grains ◽  
Weak Correlation ◽  
Interstellar Clouds ◽  
The Galaxy ◽  
The Relationship

AbstractThe relationship between DIBs and dust is still unknown. The correlation between reddening and DIB strength means that the DIBs are mixed in with the dust and gas in interstellar clouds. The DIBs are relatively stronger in the diffuse interstellar medium than in dense clouds. There is only a weak correlation between the DIBs and the UV extinction parameters including the 2175 Å bump strength and the far-UV rise. In addition, the bump dust grains are sometimes polarized, while the DIBs are not. However, observations of DIBs in the SMC show that when the 2175 Å bump is weak or missing so are the DIBs. Two of the four sightlines that deviate strongly from the CCM UV extinction in the Galaxy show weak DIBs.

scholarly journals CO2formation on interstellar dust grains: a detailed study of the barrier of the CO + O channel

2013 ◽  
Vol 559 ◽  
pp. A49 ◽  
Author(s):  
M. Minissale ◽  
E. Congiu ◽  
G. Manicò ◽  
V. Pirronello ◽  
F. Dulieu
Keyword(s):  
Interstellar Dust ◽  
Dust Grains ◽  
Interstellar Dust Grains

scholarly journals The formation of the building blocks of peptides on interstellar dust grains

2019 ◽  
Vol 15 (S350) ◽  
pp. 216-219
Author(s):  
N. F. W. Ligterink ◽  
J. Terwisscha van Scheltinga ◽  
V. Kofman ◽  
V. Taquet ◽  
S. Cazaux ◽  
...  
Keyword(s):  
Interstellar Dust ◽  
Reaction Network ◽  
Building Blocks ◽  
Dust Grains ◽  
Reaction Products ◽  
Experimental Conditions ◽  
Interstellar Dust Grains ◽  
Temperature Programmed ◽  
Life On Earth ◽  
Emergence Of Life

AbstractThe emergence of life on Earth may have its origin in organic molecules formed in the interstellar medium. Molecules with amide and isocyanate groups resemble structures found in peptides and nucleobases and are necessary for their formation. Their formation is expected to take place in the solid state, on icy dust grains, and is studied here by far-UV irradiating a CH4:HNCO mixture at 20 K in the laboratory. Reaction products are detected by means of infrared spectroscopy and temperature programmed desorption - mass spectrometry. Various simple amides and isocyanates are formed, showing the importance of ice chemistry for their interstellar formation. Constrained by experimental conditions, a reaction network is derived, showing possible formation pathways of these species under interstellar conditions.

scholarly journals LIFECYCLE OF THE INTERSTELLAR DUST GRAINS IN OUR GALAXY VIEWED WITH AKARI/MIR ALL-SKY SURVEY

2012 ◽  
Vol 27 (4) ◽  
pp. 117-122
Author(s):  
D. Ishihara ◽  
H. Kaneda ◽  
A. Mouri ◽  
T. Kondo ◽  
S. Suzuki ◽  
...  
Keyword(s):  
Interstellar Dust ◽  
Dust Grains ◽  
Interstellar Dust Grains ◽  
Sky Survey

scholarly journals Interstellar Carbon Dust

2019 ◽  
Vol 5 (4) ◽  
pp. 80
Author(s):  
Emmanuel Dartois
Keyword(s):  
Interstellar Dust ◽  
Essential Role ◽  
Carbon Budget ◽  
Remote Access ◽  
Dust Grains ◽  
Multiple Bonds ◽  
Spectroscopic Observations ◽  
Interstellar Grains ◽  
Interstellar Dust Grains ◽  
Cosmic Abundance

In the ranking of cosmic abundance of the elements, carbon is the second element, after oxygen, able to form multiple bonds propagating the formation of a network, thus playing an essential role in the formation of nanometer- to micrometer-sized interstellar dust grains. Astrophysical spectroscopic observations give us remote access to the composition of carbonaceous and organic interstellar grains. Their presence and abundances from spectroscopic observations and the phases of importance for the Galactic carbon budget are considered in this article.

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