B-Type Main-Sequence Star
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ANNUAL REPORT 2014-2015 School of Sciences and Mathematics Annual Report 2014‐2015
ANNUAL REPORT 2014-2015 School of Sciences and Mathematics Annual Report 2014‐2015 Executive Summary The 2014 – 2015 academic year was a very successful one for the School of Sciences and Mathematics (SSM). Our faculty continued their stellar record of publication and securing extramural funding, and we were able to significantly advance several capital projects. In addition, the number of majors in SSM remained very high and we continued to provide research experiences for a significant number of our students. We welcomed four new faculty members to our ranks. These individuals and their colleagues published 187 papers in peer‐reviewed scientific journals, many with undergraduate co‐authors. Faculty also secured $6.4M in new extramural grant awards to go with the $24.8M of continuing awards. During the 2013‐14 AY, ground was broken for two 3,000 sq. ft. field stations at Dixie Plantation, with construction slated for completion in Fall 2014. These stations were ultimately competed in June 2015, and will begin to serve students for the Fall 2015 semester. The 2014‐2015 academic year, marked the first year of residence of Computer Science faculty, as well as some Biology and Physics faculty, in Harbor Walk. In addition, nine Biology faculty had offices and/or research space at SCRA, and some biology instruction occurred at MUSC. In general, the displacement of a large number of students to Harbor Walk went very smoothly. Temporary astronomy viewing space was secured on the roof of one of the College’s garages. The SSM dean’s office expended tremendous effort this year to secure a contract for completion of the Rita Hollings Science Center renovation, with no success to date. -
Star Formation and Mass Assembly in High Redshift Galaxies
A&A 504, 751–767 (2009) Astronomy DOI: 10.1051/0004-6361/200811434 & c ESO 2009 Astrophysics Star formation and mass assembly in high redshift galaxies P. Santini1,2,A.Fontana1, A. Grazian1,S.Salimbeni1,3, F. Fiore1, F. Fontanot4, K. Boutsia1, M. Castellano1,2, S. Cristiani5, C. De Santis6,7, S. Gallozzi1, E. Giallongo1, N. Menci1, M. Nonino5, D. Paris1, L. Pentericci1, and E. Vanzella5 1 INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy e-mail: [email protected] 2 Dipartimento di Fisica, Università di Roma “La Sapienza”, P.le A. Moro 2, 00185 Roma, Italy 3 Department of Astronomy, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01003, USA 4 MPIA Max-Planck-Institute für Astronomie, Koenigstuhl 17, 69117 Heidelberg, Germany 5 INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy 6 Dip. di Fisica, Università Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy 7 INFN – Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Roma, Italy Received 27 November 2008 / Accepted 24 April 2009 ABSTRACT Aims. The goal of this work is to infer the star formation properties and the mass assembly process of high redshift (0.3 ≤ z < 2.5) galaxies from their IR emission using the 24 μm band of MIPS-Spitzer. Methods. We used an updated version of the GOODS-MUSIC catalog, which has multiwavelength coverage from 0.3 to 24 μmand either spectroscopic or accurate photometric redshifts. We describe how the catalog has been extended by the addition of mid-IR fluxes derived from the MIPS 24 μm image. -
FOIA Logs for US Army for 2000
Description of document: FOIA CASE LOGS for: United States Army, Alexandria, VA for 2000 - 2003 Released date: 2003 Posted date: 04-March-2008 Date/date range of document: 03-January-2000 – 27-March-2003 Source of document: Department Of The Army U.S. Army Freedom of Information and Privacy Office Casey Building, Suite 144 Attn: JDRP-RDF 7701 Telegraph Road Alexandria, VA 22315-3905 Phone: (703) 428-6494 Fax: (703) 428-6522 Email: [email protected] The governmentattic.org web site (“the site”) is noncommercial and free to the public. The site and materials made available on the site, such as this file, are for reference only. The governmentattic.org web site and its principals have made every effort to make this information as complete and as accurate as possible, however, there may be mistakes and omissions, both typographical and in content. The governmentattic.org web site and its principals shall have neither liability nor responsibility to any person or entity with respect to any loss or damage caused, or alleged to have been caused, directly or indirectly, by the information provided on the governmentattic.org web site or in this file 2000 FOIA# Rec'd Closed Susp Days Subject Refer By Control # Class AO Action 1 Action 2 Action 3 # Refer Q 00-0433 01/03/2000 04/06/2000 01/14/2000 67 Information on what the name or number of the group or company U SLF CATEGORY 9 0 S stationed in St. John's, Newfoundland during World War II in 1945 (E-Mail) 00-0434 01/03/2000 01/04/2000 01/14/2000 2 Information on the mortality rate of the former -
Durham E-Theses
Durham E-Theses First visibility of the lunar crescent and other problems in historical astronomy. Fatoohi, Louay J. How to cite: Fatoohi, Louay J. (1998) First visibility of the lunar crescent and other problems in historical astronomy., Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/996/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk me91 In the name of Allah, the Gracious, the Merciful >° 9 43'' 0' eji e' e e> igo4 U61 J CO J: lic 6..ý v Lo ý , ý.,, "ý J ýs ýºý. ur ý,r11 Lýi is' ý9r ZU LZJE rju No disaster can befall on the earth or in your souls but it is in a book before We bring it into being; that is easy for Allah. In order that you may not grieve for what has escaped you, nor be exultant at what He has given you; and Allah does not love any prideful boaster. -
Rocket Team to Discern If Our Star Count Should Go Way up | NASA
6/10/2021 Rocket Team to Discern if Our Star Count Should Go Way Up | NASA (https://www.nasa.gov/specials/apollo50th/index.html) (/multimedia/nasatv/index.html) (/) NASA TV Search Stars (/subject/6892/stars) (/sites/default/files/ciber_launch_0.jpg) Jun 3, 2021 S E I R O T S Rocket Team to Discern if Our Star Count Should Go Way Up E R UPDATE June 7, 2021: The Cosmic Infrared Background Experiment-2 or CIBER-2 was successfully launched on a NASA Black Brant O M IX sounding rocket at 2:25 a.m. EDT from the White Sands Missile Range in New Mexico. Preliminary indications show that the intended targets were viewed by the payload and good data was received. The payload flew to an apogee of about 193 miles before descending by parachute for recovery. The universe contains a mind-boggling number of stars – but scientists’ best estimates may be an undercount. A NASA-funded sounding rocket is launching with an improved instrument to look for evidence of extra stars that may have been missed in stellar head counts. The Cosmic Infrared Background Experiment-2, or CIBER-2, mission is the latest in a series of sounding rocket launches that began in 2009. Led by Michael Zemcov, assistant professor of physics and astronomy at the Rochester Institute of Technology in New York, CIBER-2’s launch window opens at the White Sands Missile Range in New Mexico on June 6, 2021. If you’ve had the pleasure of seeing an open sky on a clear, dark night, you’ve probably been struck by the sheer number of stars. -
Plotting Variable Stars on the H-R Diagram Activity
Pulsating Variable Stars and the Hertzsprung-Russell Diagram The Hertzsprung-Russell (H-R) Diagram: The H-R diagram is an important astronomical tool for understanding how stars evolve over time. Stellar evolution can not be studied by observing individual stars as most changes occur over millions and billions of years. Astrophysicists observe numerous stars at various stages in their evolutionary history to determine their changing properties and probable evolutionary tracks across the H-R diagram. The H-R diagram is a scatter graph of stars. When the absolute magnitude (MV) – intrinsic brightness – of stars is plotted against their surface temperature (stellar classification) the stars are not randomly distributed on the graph but are mostly restricted to a few well-defined regions. The stars within the same regions share a common set of characteristics. As the physical characteristics of a star change over its evolutionary history, its position on the H-R diagram The H-R Diagram changes also – so the H-R diagram can also be thought of as a graphical plot of stellar evolution. From the location of a star on the diagram, its luminosity, spectral type, color, temperature, mass, age, chemical composition and evolutionary history are known. Most stars are classified by surface temperature (spectral type) from hottest to coolest as follows: O B A F G K M. These categories are further subdivided into subclasses from hottest (0) to coolest (9). The hottest B stars are B0 and the coolest are B9, followed by spectral type A0. Each major spectral classification is characterized by its own unique spectra. -
SHELL BURNING STARS: Red Giants and Red Supergiants
SHELL BURNING STARS: Red Giants and Red Supergiants There is a large variety of stellar models which have a distinct core – envelope structure. While any main sequence star, or any white dwarf, may be well approximated with a single polytropic model, the stars with the core – envelope structure may be approximated with a composite polytrope: one for the core, another for the envelope, with a very large difference in the “K” constants between the two. This is a consequence of a very large difference in the specific entropies between the core and the envelope. The original reason for the difference is due to a jump in chemical composition. For example, the core may have no hydrogen, and mostly helium, while the envelope may be hydrogen rich. As a result, there is a nuclear burning shell at the bottom of the envelope; hydrogen burning shell in our example. The heat generated in the shell is diffusing out with radiation, and keeps the entropy very high throughout the envelope. The core – envelope structure is most pronounced when the core is degenerate, and its specific entropy near zero. It is supported against its own gravity with the non-thermal pressure of degenerate electron gas, while all stellar luminosity, and all entropy for the envelope, are provided by the shell source. A common property of stars with well developed core – envelope structure is not only a very large jump in specific entropy but also a very large difference in pressure between the center, Pc, the shell, Psh, and the photosphere, Pph. Of course, the two characteristics are closely related to each other. -
Ioptron AZ Mount Pro Altazimuth Mount Instruction
® iOptron® AZ Mount ProTM Altazimuth Mount Instruction Manual Product #8900, #8903 and #8920 This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while observing. 2 Table of Content Table of Content ......................................................................................................................................... 3 1. AZ Mount ProTM Altazimuth Mount Overview...................................................................................... 5 2. AZ Mount ProTM Mount Assembly ........................................................................................................ 6 2.1. Parts List .......................................................................................................................................... 6 2.2. Identification of Parts ....................................................................................................................... 7 2.3. Go2Nova® 8407 Hand Controller .................................................................................................... 8 2.3.1. Key Description ....................................................................................................................... -