Materials Map

Discover the materials research landscape. Find experts, partners, networks.

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The Materials Map is an open tool for improving networking and interdisciplinary exchange within materials research. It enables cross-database search for cooperation and network partners and discovering of the research landscape.

The dashboard provides detailed information about the selected scientist, e.g. publications. The dashboard can be filtered and shows the relationship to co-authors in different diagrams. In addition, a link is provided to find contact information.

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Materials Map under construction

The Materials Map is still under development. In its current state, it is only based on one single data source and, thus, incomplete and contains duplicates. We are working on incorporating new open data sources like ORCID to improve the quality and the timeliness of our data. We will update Materials Map as soon as possible and kindly ask for your patience.

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in Cooperation with on an Cooperation-Score of 37%

Topics

Publications (6/6 displayed)

  • 2019Dust scaling relations in a cosmological simulation65citations
  • 2019Dust scaling relations in a cosmological simulationcitations
  • 2018Cosmological simulation with dust formation and destruction91citations
  • 2018Populating H<SUB>2</SUB> and CO in galaxy simulation with dust evolution28citations
  • 2017Evolution of dust extinction curves in galaxy simulation49citations
  • 2017Galaxy simulation with dust formation and destruction111citations

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Nagamine, Kentaro
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Hou, Kuan-Chou
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Aoyama, Shohei
6 / 7 shared
Hirashita, Hiroyuki
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Chen, Li-Hsin
1 / 1 shared
Choi, Jun-Hwan
1 / 1 shared
Todoroki, Keita
1 / 1 shared
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2019
2018
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Co-Authors (by relevance)

  • Nagamine, Kentaro
  • Hou, Kuan-Chou
  • Aoyama, Shohei
  • Hirashita, Hiroyuki
  • Chen, Li-Hsin
  • Choi, Jun-Hwan
  • Todoroki, Keita
OrganizationsLocationPeople

article

Evolution of dust extinction curves in galaxy simulation

  • Nagamine, Kentaro
  • Hou, Kuan-Chou
  • Shimizu, Ikkoh
  • Aoyama, Shohei
Abstract

To understand the evolution of extinction curve, we calculate the dust evolution in a galaxy using smoothed particle hydrodynamic simulations incorporating stellar dust production, dust destruction in supernova shocks, grain growth by accretion and coagulation, and grain disruption by shattering. The dust species are separated into carbonaceous dust and silicate. The evolution of grain size distribution is considered by dividing grain population into large and small grains, which allows us to estimate extinction curves. We examine the dependence of extinction curves on the position, gas density and metallicity in the galaxy, and find that extinction curves are flat at t ≲ 0.3 Gyr because stellar dust production dominates the total dust abundance. The 2175 Å bump and far-ultraviolet (FUV) rise become prominent after dust growth by accretion. At t ≳ 3 Gyr, shattering works efficiently in the outer disc and low-density regions, so extinction curves show a very strong 2175 Å bump and steep FUV rise. The extinction curves at t ≳ 3 Gyr are consistent with the Milky Way extinction curve, which implies that we successfully included the necessary dust processes in the model. The outer disc component caused by stellar feedback has an extinction curve with a weaker 2175 Å bump and flatter FUV slope. The strong contribution of carbonaceous dust tends to underproduce the FUV rise in the Small Magellanic Cloud extinction curve, which supports selective loss of small carbonaceous dust in the galaxy. The snapshot at young ages also explains the extinction curves in high-redshift quasars....

Topics
  • density
  • impedance spectroscopy
  • grain
  • grain size
  • simulation
  • grain growth