Home | Contact | Sitemap | 中文 | CAS
About Us Research People International Cooperation News Education & Training Join Us Journals Papers Resources Links
Location: Home > News > Seminars
  • Events
  • Seminars
  • Research Trends
  • The Origins of Young Stars in the Direction of Leading Arm of the Magellanic Stream

    Seminar Title  

    The Origins of Young Stars in the Direction of Leading Arm of the Magellanic Stream

    Speaker:  Dr. ZHANG Lan




    Tuesday afternoon, July 2, 14:00 p.m.



    Room 208 No.2 building , Xianlin campus (PMO, CAS)

                             Welcome to Attend   

      ( PMO Academic Committee & Academic Circulating committee)


    Abstract We explore the origins of the young B-type stars found by Casetti-Dinescu et al. (2014) at the outskirts of the Milky-Way disk in the sky region of Leading Arm of the Magellanic Stream. High-resolution spectroscopic observations made with the MIKE instrument on the Magellan Clay 6.5m telescope for nine stars are added to the previous sample analyzed by Zhang et al. (2017). We compile a sample of fifteen young stars with well-determined stellar types, ages, abundances and kinematics. With proper motions from Gaia DR2 we also derive orbits in a realistic Milky-Way potential. We find that our previous radial-velocity selected LA candidates have substantial orbital angular momentum. The substantial amount of rotational component for these stars is in contrast with the near-polar Magellanic orbit, thus rendering these stars unlikely members of the LA. There are four large orbital-energy stars in our sample. The highest orbital-energy one has an age shorter than the time to disk crossing, with a birthplace z=2.5 kpc and R_GC ~28 kpc. Therefore, the origin of this star is uncertain. The remaining three stars have disk runaway origin with birthplaces between 12 and 25 kpc from the Galactic center. Also, the most energetic stars are more metal poor ([Mg/H] =-0.50+/-0.07) and with larger He scatter (sigma_[He/H] = 0.72) than the inner disk ones ([Mg/H] =0.12+/-0.36, sigma_[He/H] = 0.15). While the former group's abundance is compatible with that of the Large Magellanic Cloud, it could also reflect the metallicity gradient of the MW disk and their runaway status via different runaway mechanisms.
     Zhang Lan, research associate at Stellar Abundance and Galaxy Evolution Group, NAOC. Lan’s research field covers abundances and kinematics of the Milky Way, Galactic formation and evolution, data analysis of laboratory astrophysics etc. Zhang Lan obtained her PhD in 2012.
    Copyright ? Purple Mountain Observatory, CAS, No.10 Yuanhua Road, Qixia District, Nanjing 210033, China
    Phone: 0086 25 8333 2000 Fax: 8333 2091 http://english.pmo.cas.cn