PPT-Effects of Stellar Variability:

1 28 Important for transits see next slides Transit depth R planet λ t R star λt 2 Not so important for eclipses because the eclipse is a simple difference and the stellar variability typically is slower than the eclipse . of Sun-like stars. (“solar variability after dark”). Wes Lockwood, Lowell Observatory. Gregory Henry, TSU. Robotic photometry 1993-2014. Tennessee State Univ. telescopes at Fairborn Observatory. Lou Boyd, input. . atmospheres. a . very. . short. . introduction. Part I. Ewa Niemczura. Astronomical. . Institute. , . UWr. eniem@astro.uni.wroc.pl. Stellar. spectra. Stellar. spectra. One picture is worth 1000 words, but . . Greg . Feiden. & Brian . Chaboyer (Dartmouth). Three color EUV image of the Sun. White lines show a model of the Sun’s magnetic field . (. Schrijver. & Title 2011). Measurements of average magnetic fields in M dwarfs. Mark Morris. UCLA. ABSTRACT -- The . well-defined, massive disk of young stars orbiting within 0.5 pc of the Galactic black hole (GBH) is strongly tilted with respect to the Galactic plane. In the context of in situ formation mechanisms, this orientation is inherited from that of the gas disk that formed these stars on the order of 6 million years ago. The tilt can be understood by positing that clouds fall toward the GBH on near-zero angular momentum orbits and form dispersion rings as they self-intersect after . young stars . with . LSST. Gregory J. Herczeg. KIAA. Star Formation: . ISM/Molecular Clouds . Pre-main sequence stellar evolution. (low-mass case). HD141569, . Clampin. et al.. Classical T . Tauri. Stars. Giuseppina. . Battaglia. Instituto. de . Astrofisica. de Canarias, Tenerife. Credit. : ESO/. H.H.Heyer. Credit. : ESO/L. . Calçada. Karachentsev. et al. 2014. Individual . Red . Giant Branch . stars. Soroush Sotoudeh. . (University of Minnesota). Daniel . Weisz. , Andrew Dolphin, Evan Skillman. 06/29/2015 – . STScI. Workshop on IMF. Outline. Introduction. Observations and data. IMF analysis and results. Matthew Lave and Jan Kleissl. Solar 2011. Variability Reduction through Aggregation. Relative Output. Large ramps are detectable real-time by satellite and ground stations. Variability models primarily needed for large central power plants / . Bureau . of Meteorology – R&D Branch. Regional characteristics of tropical expansion and the role of climate variability. Observations vs Models. Observed rate in many metrics is 0.5 – 1.0 degrees/decade of expansion. Kepler. . AutoRegressive. Planet Search. Eric . Feigelson & . Gabriel Caceres. Penn State Astronomy & Astrophysics. with . statisticians G. . . J. . Babu. , N. . Bahamonde. , . K. . . Bertin. Transiting Exoplanets. Dainis Dravins. 1. , . Hans-Günter Ludwig. 2. ,. Erik Dahlén. 1. ,. Martin Gustavsson. 1. , . Hiva. Pazira. 1. . 1. . Lund Observatory, Sweden, . 2. . Landessternwarte. JEFFREY HALL. LOWELL OBSERVATORY, FLAGSTAFF, AZ. Project Timeline. 1988 1992 1996 2000 2004 2008 2012 . Construction/early observing. Rebuild 1. Broad survey. Solar analog survey. Rebuild 2. A/D boundary. Swift. -BAT blazars with . NICER. Sergio Mundo, Richard . Mushotzky. University of Maryland, College Park. MARLAM 9, JHU, Baltimore, MD. Blazar characteristics. Radio-loud AGN with jet aligned close to line of sight. Matthew DeLand. 1. 1. Science Systems and Applications, Inc. (SSAI). Impacts of Intermediate Time Scale SSI Variability Workshop. 9 December 2018, Columbia, MD. Definition of “Short-Term SSI Variability”.