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Stellar Dynamics and Stellar Phenomena Near a Massive Black Hole
Stellar Dynamics and Stellar Phenomena Near A Massive Black Hole Tal Alexander Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, Rehovot, Israel 76100; email: [email protected] | Author's original version. To appear in Annual Review of Astronomy and Astrophysics. See final published version in ARA&A website: www.annualreviews.org/doi/10.1146/annurev-astro-091916-055306 Annu. Rev. Astron. Astrophys. 2017. Keywords 55:1{41 massive black holes, stellar kinematics, stellar dynamics, Galactic This article's doi: Center 10.1146/((please add article doi)) Copyright c 2017 by Annual Reviews. Abstract All rights reserved Most galactic nuclei harbor a massive black hole (MBH), whose birth and evolution are closely linked to those of its host galaxy. The unique conditions near the MBH: high velocity and density in the steep po- tential of a massive singular relativistic object, lead to unusual modes of stellar birth, evolution, dynamics and death. A complex network of dynamical mechanisms, operating on multiple timescales, deflect stars arXiv:1701.04762v1 [astro-ph.GA] 17 Jan 2017 to orbits that intercept the MBH. Such close encounters lead to ener- getic interactions with observable signatures and consequences for the evolution of the MBH and its stellar environment. Galactic nuclei are astrophysical laboratories that test and challenge our understanding of MBH formation, strong gravity, stellar dynamics, and stellar physics. I review from a theoretical perspective the wide range of stellar phe- nomena that occur near MBHs, focusing on the role of stellar dynamics near an isolated MBH in a relaxed stellar cusp. -
Dark Mater Compact Stars in Pseudo-Complex General Relativity]{Dark Mater Compact Stars in Pseudo-Complex General Relativity
Dark Mater Compact Stars in Pseudo-Complex General Relativity]{Dark Mater Compact Stars in Pseudo-Complex General Relativity César A. Zen Vasconcellos Instituto de Física Universidade Federal do Rio Grande do Sul (UFRGS) Porto Alegre, RS, Brazil E-mail: [email protected] Abstract: In the theory of pseudo-complex General Relativity (pc-GR), the field equations have an extra term, associated to the nature of spacetime, of repulsive character, which is believed to halt the gravitational attractive collapse of matter distributions in the evolution process of compact stars. According to Walter Greiner and Peter Hess, this additional term arises from micro-scale phenomena due to vacuum fluctuations which simulate the presence of dark energy in the Universe. In this contribution we explore the presence of this additional term and propose a toy model consisting of dark matter, represented by Standard Model gauge singlets having their origin in a portal model, held together by the presence of the gravitational interaction and superimposed to this (repulsive) background of dark energy forming a type of unconventional and non-luminous star. The combination of these two ingredients, gravitational attraction and dark energy repulsion, allows in thesis the hydrostatic equilibrium condition of the star to hold. Solving the corresponding field equations and the TOV equations, and assuming that the fluid components interact only gravitationally, we determine the hydrostatic equilibrium equations of the star composed only by dark matter and dark energy, a rare compact object formed solely by exotic content. We them analyze the corresponding results obtained for the equation of state and for the mass-radius relations and we them determine the maximum mass of the exotic star for different parameter configurations.. -
Works of Love
reader.ad section 9/21/05 12:38 PM Page 2 AMAZING LIGHT: Visions for Discovery AN INTERNATIONAL SYMPOSIUM IN HONOR OF THE 90TH BIRTHDAY YEAR OF CHARLES TOWNES October 6-8, 2005 — University of California, Berkeley Amazing Light Symposium and Gala Celebration c/o Metanexus Institute 3624 Market Street, Suite 301, Philadelphia, PA 19104 215.789.2200, [email protected] www.foundationalquestions.net/townes Saturday, October 8, 2005 We explore. What path to explore is important, as well as what we notice along the path. And there are always unturned stones along even well-trod paths. Discovery awaits those who spot and take the trouble to turn the stones. -- Charles H. Townes Table of Contents Table of Contents.............................................................................................................. 3 Welcome Letter................................................................................................................. 5 Conference Supporters and Organizers ............................................................................ 7 Sponsors.......................................................................................................................... 13 Program Agenda ............................................................................................................. 29 Amazing Light Young Scholars Competition................................................................. 37 Amazing Light Laser Challenge Website Competition.................................................. 41 Foundational -
Reversed out (White) Reversed
Berkeley rev.( white) Berkeley rev.( FALL 2014 reversed out (white) reversed IN THIS ISSUE Berkeley’s Space Sciences Laboratory Tabletop Physics Bringing More Women into Physics ALUMNI NEWS AND MORE! Cover: The MAVEN satellite mission uses instrumentation developed at UC Berkeley's Space Sciences Laboratory to explore the physics behind the loss of the Martian atmosphere. It’s a continuation of Berkeley astrophysicist Robert Lin’s pioneering work in solar physics. See p 7. photo credit: Lockheed Martin Physics at Berkeley 2014 Published annually by the Department of Physics Steven Boggs: Chair Anil More: Director of Administration Maria Hjelm: Director of Development, College of Letters and Science Devi Mathieu: Editor, Principal Writer Meg Coughlin: Design Additional assistance provided by Sarah Wittmer, Sylvie Mehner and Susan Houghton Department of Physics 366 LeConte Hall #7300 University of California, Berkeley Berkeley, CA 94720-7300 Copyright 2014 by The Regents of the University of California FEATURES 4 12 18 Berkeley’s Space Tabletop Physics Bringing More Women Sciences Laboratory BERKELEY THEORISTS INVENT into Physics NEW WAYS TO SEARCH FOR GOING ON SIX DECADES UC BERKELEY HOSTS THE 2014 NEW PHYSICS OF EDUCATION AND SPACE WEST COAST CONFERENCE EXPLORATION Berkeley theoretical physicists Ashvin FOR UNDERGRADUATE WOMEN Vishwanath and Surjeet Rajendran IN PHYSICS Since the Space Lab’s inception are developing new, small-scale in 1959, Berkeley physicists have Women physics students from low-energy approaches to questions played important roles in many California, Oregon, Washington, usually associated with large-scale of the nation’s space-based scientific Alaska, and Hawaii gathered on high-energy particle experiments. -
The History of Enrichment of the Intergalactic Medium Using Cosmological Simulations
The History of Enrichment of the Intergalactic Medium Using Cosmological Simulations Item Type text; Electronic Dissertation Authors Oppenheimer, Benjamin Darwin Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 03/10/2021 02:22:25 Link to Item http://hdl.handle.net/10150/194237 THE HISTORY OF ENRICHMENT OF THE INTERGALACTIC MEDIUM USING COSMOLOGICAL SIMULATIONS by Benjamin Darwin Oppenheimer A Dissertation Submitted to the Faculty of the DEPARTMENT OF ASTRONOMY In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 2 0 0 8 2 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Dissertation Committee, we certify that we have read the dissertation prepared by Benjamin Darwin Oppenheimer entitled “The History of Enrichment of the Intergalactic Medium Using Cosmological Simulations” and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Philosophy. Date: August 6, 2008 Romeel Dave´ Date: August 6, 2008 Chris Impey Date: August 6, 2008 Jill Bechtold Date: August 6, 2008 Buell Jannuzi Date: August 6, 2008 John Bieging Final approval and acceptance of this dissertation is contingent upon the candi- date's submission of the final copies of the dissertation to the Graduate College. I hereby certify that I have read this dissertation prepared under my direction and recommend that it be accepted as fulfilling the dissertation requirement. -
Newsletter Submillimeter Array Newsletter Number 20 | July 2015
SMA Newsletter Submillimeter Array Newsletter Number 20 | July 2015 CONTENTS FROM THE DIRECTOR 1 From the Director SCIENCE HIGHLIGHTS: Dear SMA Newsletter readers, 2 Nuclear Ashes and Outflow in the Eruptive Star Nova I am pleased to congratulate Thomas Kaminski (ESO Chile and MPI Bonn), Hua-Bai Vul 1670 Li (The Chinese University of Hong Kong), Jean Turner (UCLA) and their colleagues 5 Magnetic Fields Shape for their recent publications in Nature, summarized in this Newsletter. Collectively Molecular Cloud Structures 7 A Cosmic Factory of Stars these publications highlight the relative ease and utility of the SMA to observe bright, and Soot – SMA Reveals a chemically rich, galactic sources, and nearby galaxies; and further demonstrate the SMA’s Super Star Cluster of Highly Efficient Star Formation in relatively unique polarization capability. NGC 5253 I would also like to thank members of the SMA correlator group for their continued efforts TECHNICAL HIGHLIGHTS: to provide additional wideband signal-processing capacity. We now regularly observe with bu A SWARM of ROACHs the first tranche of SWARM, albeit at 3/4 speed, in parallel with the aging ASIC correlator, Has Been Deployed for Submillimeter Array Science in service since 2002. While not yet perfect, the additional 2x1.5 GHz bands, coupled with bp Securing Service - Availability the original 2x2 GHz bands of the ASIC correlator and double sideband receiver operation in Hawaii Using Virtual Infrastructure result in an instantaneous bandwidth of 14 GHz. This provides additional flexibility OTHER NEWS during spectral line observations and improves the continuum sensitivity of the SMA by about 40%. -
Gravity-Superconductor Interactions
id2441218 pdfMachine by Broadgun Software - a great PDF writer! - a great PDF creator! - http://www.pdfmachine.com http://www.broadgun.com Mehtapress 2013 Print - ISSN : 2319–9814 Journal of Online - ISSN : 2319–9822 SpFauclle pEapxepr loration Full Paper WWW.MEHTAPRESS.COM P.A.Murad* An assessment concerning neutron stars and Morningstar Applied Physics, LLC, space propulsion implications Vienna, VA 22182, (USA) E-mail: [email protected] PACS: 04.50.Kd, 04.80.Cc, 06.30.Dr, Abstract 06.30. Gv, 97.10.-q, 97.10.Gz, 97.10.Xq, 97.60.Gb, 97.60.Jd, 97.60.Lf, 97.80.-d There are many uncertainties concerning stellar evolution of neutron stars. Neutron stars might possess multipolar architecture in lieu of a single dipole claimed by the conventional wisdom. The multipole issue cannot be resolved using a single observer reference point Received: April 30, 2013 such as the Earth, but would require an additional non-terrestrial observer location with a Accepted: June 24, 2013 significant offset. Without observing multiple beacons, we could not verify or deny the Published: July 29, 2013 existence of multiple poles from observing the sweeping lighthouse effect from Earth. Moreover, a neutron star’s magnetic field may be created by differences between the neutron core and a gas surface layer of protons and electrons. These differences between *Corresponding author’s Name & Add. the layers constitute charges and moving currents that result in a magnetic field supported by a fast moving rotating core. If electrons in Cooper pairs exist in a neutron star, then the amount of magnetism may increase by a similar order via superconductivity. -
The Observatory Founded in 1877 by Sir William Christie, Astronomer Royal
The Observatory Founded in 1877 by Sir William Christie, Astronomer Royal EditEd by D. J. SticklanD R. W. ARgyle S. J. Fossey eDitors 1877–2013 W. H. m. Christie 1877–1882 P. J. d. Gething 1954–1956 E. W. maunder 1881–1887 d. W. dewhirst 1956–1957 A. m. W. downing 1885–1887 A. Hewish 1957–1961 t. lewis 1885–1887 W. R. Hindmarsh 1957–1961 and 1893–1912 b. E. J. Pagel 1961–1962 A. A. Common 1888–1892 J. E. baldwin 1961–1962 H. H. turner 1888–1897 d. mcNally 1961–1963 H. P. Hollis 1893–1912 C. A. murray 1961–1966 S. Chapman 1913–1914 P. A. Wayman 1962–1964 A. S. Eddington 1913–1919 R. V. Willstrop 1963–1966 F. J. m. Stratton 1913–1925 R. F. Griffin 1963–1985 H. Spencer Jones 1915–1923 J. b. Alexander 1964–1965 J. Jackson 1920–1927 S. V. m. Clube 1965–1966 W. m. H. Greaves 1924–1932 K. b. Gebbie 1966–1968 J. A. Carroll 1926–1931 W. Nicholson 1966–1973 G. merton 1928 d. lynden-bell 1967–1969 W. H. Steavenson 1929–1933 C. Jordan 1968–1973 H. W. Newton 1929–1936 R. G. bingham 1969–1972 R. o. Redman 1932–1935 m. V. Penston 1972–1975 R. v. d. R. Woolley 1933–1939 S. J. burnell 1973–1976 W. H. mcCrea 1935–1937 d. H. P. Jones 1973–1977 H. F. Finch 1936–1947 P. J. Andrews 1975–1983 A. d. thackeray 1938–1942 G. G. Pooley 1976–1984 G. C. mcVittie 1938–1948 R. -
Jocelyn Bell Burnell
Jocelyn Bell Burnell President of the Royal Astronomical Society 2002 to 2004 President of the Institute of Physics 2008 to 2010 Elected Pro-Chancellor of the University of Dublin 2013 Elected President of the Royal Society of Edinburgh 2014 B.S University of Glasgow (1965) Ph.D., Radio Astronomy, University of Cambridge (1968) Biography Jocelyn Bell Burnell was born in 1943 in Northern Ireland to Allison and Phillip Bell. She discovered her passion for astronomy early in life through books. At Lurgan College, she began her higher education but was restricted from studying science due to her gender. At the time, women were not allowed to study science at the school. Her parents were committed to the education of their daughter so when Jocelyn was unable to pass the entrance examine for continuing education her parents sent her to a Quaker boarding school. At the age of 22, she graduated from the University of Glasgow with a degree in Physics and then went on to earn her doctorate at the University of Cambridge. Presently she is working as a visiting Professor or Astrophysics at the University of Oxford. Research Jocelyn Bell Brunell’s groundbreaking research began during her time at Cambridge. She was involved in the development of a radio telescope to track quasars and after its completion became the telescope operator in charge of analyzing data collected. It was during this time that she discovered an anomaly in the data, which led her to the discovery of pulsars. This discovery lead to the 1974 Nobel Prize in Physics awarded to the lead researcher Antony Hewish along with Marti Ryle. -
Reinhard Genzel
Reinhard Genzel Date of Birth 24 March 1952 Place Bad Homburg v.d.H., Germany Nomination 18 August 2020 Field Physics; Astronomy Title Director at the Max Planck Institute for Extraterrestrial Physics, Garching, Germany; Nobel Laureate in Physics, 2020 Most important awards, prizes and academies Awards and Honors: 1970 Alfred Maul Medal, Bertold Gymnasium, Freiburg, Germany; 1973 Scholarship of the "Studienstiftung des Deutschen Volkes", Germany; 1980 Otto Hahn Medal of the Max Planck Society for the Year 1978, Germany; 1980 Miller Fellowship, University of California, Berkeley, USA; 1984 Presidential Young Investigators Award, USA; 1985 Fellow, American Physical Society, USA; 1986 Newton Lacy Pierce Prize, American Astronomical Society, USA; 1990 Leibniz Prize of the German Science Foundation (DFG), Germany; 1998 Foreign Member, Académie des Sciences, Paris, France; 2000 de Vaucouleurs Medal, University of Texas, Austin, USA; 2000 Foreign Associate, US National Academy of Sciences, USA; 2000 Janssen Prize, Société Astronomique de France, Paris, France; 2002 Member of the German Academy of Natural Sciences Leopoldina, Halle, Germany; 2002 Member of the European Academy of Sciences, Liège, Belgium; 2003 Stern Gerlach Medal of the German Physical Society (DPG), Germany; 2003 Member of the Bavarian Academy of Sciences, Munich, Germany; 2003 Balzan Prize for ’Infrared Astronomy’, Bern, Switzerland/Italy; 2005 Petrie Prize, Canadian Astronomical Society (CASCA), Victoria, Canada; 2007 Einstein Medal, Albert Einstein Society (AEG), Bern, Switzerland; -
Phase Transitions in Neutron Stars and Their Links to Gravitational Waves
Phase transitions in neutron stars and their links to gravitational waves Milva G. Orsaria 1;2, Germ´anMalfatti 1;2, Mauro Mariani 1;2, Ignacio F. Ranea-Sandoval 1;2, Federico Garc´ıa 4;5, William M. Spinella 6, Gustavo A. Contrera 1;3;8, Germ´anLugones 7, and Fridolin Weber 8;9 1Grupo de Gravitaci´on,Astrof´ısicay Cosmolog´ıa,Facultad de Ciencias Astron´omicasy Geof´ısicas,Univer- sidad Nacional de La Plata, Paseo del Bosque S/N, 1900, La Plata, Argentina. 2 CONICET, Godoy Cruz 2290, 1425, CABA, Argentina. 3 IFLP, UNLP, CONICET, Facultad de Ciencias Exactas, Diagonal 113 e/63 y 64, 1900, La Plata, Argentina. 4 AIM, CEA, CNRS, Universit´eParis-Saclay, Universit´eParis Diderot, Sorbonne Paris Cit´e,F-91191 Gif-sur- Yvette, France. 5 Instituto Argentino de Radioastronom´ıa(CCT-La Plata, CONICET; CICPBA), C.C. No. 5, 1894 Villa Elisa, Argentina. 6 Department of Sciences, Wentworth Institute of Technology, 550 Huntington Avenue, Boston, MA 02115, USA. 7 Universidade Federal do ABC, Centro de Ci^enciasNaturais e Humanas, Avenida dos Estados 5001- Bang´u, CEP 09210-580, Santo Andr´e,SP, Brazil. 8 Department of Physics, San Diego State University, San Diego, CA 92182, USA. 9 University of California at San Diego, La Jolla, CA 92093, USA. Abstract The recent direct observation of gravitational wave event GW 170817 and its GRB170817A signal has opened up a new window to study neutron stars and heralds a new era of Astronomy referred to as the Multimessenger Astronomy. Both gravitational and electromagnetic waves from a single astrophysical source have been detected for the first time. -
Bursts of Gravitational Waves Due to Crustquake from Pulsars
J. Astrophys. Astr. (0000) 000: #### DOI Bursts of Gravitational Waves due to Crustquake from Pulsars Biswanath Layek1,* and Pradeepkumar Yadav1 1Birla Institute of Technology and Science, Pilani Campus Pilani, Jhunjhunu 333031, Rajasthan, India *Corresponding author. E-mail: [email protected] Abstract. We revisit here a possibility of generation of gravitational wave (GW) bursts due to a very quick change in the quadrupole moment (QM) of a deformed spheroidal pulsar as a result of crustquake. Since it was originally proposed as a possible explanation for sudden spin-up (glitch) of pulsars, the occurrence of crustquake and it’s various consequences have been studied and discussed quite often in the literature. Encouraged by recent development in gravitational wave (GW) astronomy, we re-investigate the role of crustquake in the emission of GWs. Assuming exponential decay of excitation caused by crustquake, we have performed a Fourier analysis to estimate the GW strain amplitude h(t), characteristic signal amplitude hc( f ) and signal to noise ratio (SNR) of the burst for the Crab pulsar. For exotic quark stars, multifold enhancement of these quantities are expected, which might make quark star a potential source of gravitational waves. The absence of such bursts may put several constraints on pulsars and such hypothetical stars. Keywords. Neutron Star, Pulsar, Crustquake, Gravitational wave. 1. Introduction mal modes of a pulsar and hence may emit GWs. The timing glitch can be one of these sources, which has The remarkable first-ever direct detection of GWs in the potential to excite quasinormal modes in the parent 2015 by LIGO (Abbott & et al.