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워크숍/세미나

Cosmic Dust & Magnetism conference

Cosmic Dust & Magnetism conference

  • 행사기간 : 2018년 10월 30일 ~ 11월 2일
  • 장소 : LWC Hall 1st floor Room #102, KASI
  • 주최 : Theoretical Astrophysics Group / 주관 : Theoretical Astrophysics Group
  • 문의 : Dr. Thiem Hoang(thiemhoang@kasi.re.kr) and Dr. Jinho Kim(jkim@kasi.re.kr)
개요

Dust and magnetic fields are ubiquitous in the universe. Interstellar dust is the seeds of star and planet formation, while magnetic fields play an important role in many astrophysical phenomena, including star formation, cosmic ray transport, and synchrotron emission. The alignment of non-spherical dust grains with magnetic fields, resulting in dust polarization, provides a powerful tool to map magnetic fields. Dust polarization has been successfully used to trace magnetic fields in various scales, from ~ kpc to ~ 1000 AU scales. Recent polarization observations at mm-cm wavelengths from disks (~ 100 AU scales) by ALMA reveal that dust polarization may not trace magnetic fields, but grain growth and planetesimal formation. At the same time, polarized dust emission is considered the most critical challenge for understanding how the universe was born through so-called B-modes polarization. Therefore, accurate modeling of dust foreground polarization, which depends on dust astrophysics, gas density, and magnetic field structure, is required for the B-modes detection. The aim of this workshop is to bring together local and international experts in dust astrophysics and magnetic fields in order to discuss the following important aspects: 


1. Dust Properties and Dust Evolution from Angstroms to centimeters to planetesimals 

2. Physics of Dust Polarization: grain alignment, scattering, and observational tests

3. What is the role of magnetic fields on star and planet formation?

4. What can we learn from mm-cm dust polarization observations in the ALMA era: Magnetic fields or Grain Growth?

5. Alternative ways to trace magnetic fields as a synergy to dust polarization

6. Related important issues: turbulence, filaments, and shocks 

7. What dust astrophysics and magnetic fields required for accurate modeling of Galactic foreground for CMB B-modes detection?


▶ Conference Website:  http://coma.kasi.re.kr/cosdm2018

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후기 및 결과


만족도 조사
콘텐츠 담당부서우주과학본부,우주측지그룹,고천문연구센터
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