PPT-Spectral Properties of Superflare Stars, KIC 9766237, and K

Daisaku Nogami Kyoto University 20140123Thu Subaru Users Meeting 2013NAOJ Collaborators K Shibata H Maehara S Honda T Shibayama S Notsu Y . Stoica R Moses Spectral analysis of signals available online at httpuserituuse psSASnewpdf 2 14 brPage 3br Deterministic signals Power spectral density de64257nitions Power spectral density properties Power spectral estimation Goal Given a 64257ni . on Solar type Stars and Their Impacts on Habitability of . Exoplanets. Kazunari. Shibata. . Kwasan. and . Hida. observatories, . Kyoto University. Hiroaki Isobe. Unit of Synergetic Studies for Space, Kyoto University. . Gray and . Corbally. Chapter 8 . Karen Garcia. Georgia State University. Outline. Basic characteristics. Spectral . f. eatures. Mira variables. Carbon stars. The First Step in Quantitative Spectral Analysis. Richard Gray. Appalachian State University. MK Spectral Classification: 1943 – 2013. 70 years of contributions to stellar astronomy. Discovery of the spiral structure of the Galaxy (Morgan, . Suggest Variable Star Universality. John F. . L. indner, Wooster College. Presented by . John . G. Learned. University of Hawai’i at Mānoa. Collaboration. John F. Lindner. The College of Wooster. Vivek Kohar. biotissues. D.A. Loginova. 1,2. , E.A. Sergeeva. 1. , P.D. Agrba. 2. , . and M. Yu. Kirillin. 1. 1 . Institute of Applied Physics RAS, Nizhny Novgorod, Russia. 2 . Lobachevsky. State University of Nizhny Novgorod, Nizhny Novgorod, Russia. biotissues. D.A. Loginova. 1,2. , E.A. Sergeeva. 1. , P.D. Agrba. 2. , . and M. Yu. Kirillin. 1. 1 . Institute of Applied Physics RAS, Nizhny Novgorod, Russia. 2 . Lobachevsky. State University of Nizhny Novgorod, Nizhny Novgorod, Russia. Ursa. Minor (Little Dipper). Ursa. Major (Big Dipper). Cassieopa. Cepheus. Draco. Orion. Bootes. Capella. Castor & . Pollux. (Gemini). Corona Borealis. Saggitarius. Hercules. Fomahault. (Pieces). Chapter 17. How do stars differ? Is . the Sun typical?. Image . of Orion illustrates:. The huge number of stars. Colors. Interstellar . gas. How can we describe/classify stars. ?. Location. Temperature. Ultra Metal - Poor (UMP ; [Fe/H] - 4 . 0 ) stars hold the key to the nucleosynthesis processes associated with first - generation stars in the Universe . However, only about two dozen UMP stars have b Stars form in a cloud of dust and gas in space called a nebula.. How do stars form?. A force from outside the nebula causes the cloud to condense into stars. . Example: a shockwave. Gravity causes the particle in the cloud to contract.. MASSIVE STARS. b. y. . Ph. Stee. Massive Stars sub-group:. Borges . Fernandes. Marcelo. Carciofi. Alex. de Wit Willem-Jan . Domiciano. de Souza Armando. Faes. Daniel. Kostogryz. Nadia . Meilland. Daisaku Nogami (Kyoto University). 2014/01/23(Thu). Subaru User's Meeting 2013@NAOJ. Collaborators: K. Shibata, H. . Maehara. , S. Honda, T. . Shibayama. ,. S. . Notsu. , Y. . Exoplanets. Kazunari. Shibata. . Kwasan. and . Hida. observatories, . Kyoto University. Hiroaki Isobe. Unit of Synergetic Studies for Space, Kyoto University. isobe@kwasan.kyoto. -. u.ac.jp. COSPAR2014, .