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by: Danielle Moore


Danielle Moore
GPA 3.61


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Class Notes
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This 37 page Class Notes was uploaded by Danielle Moore on Saturday September 12, 2015. The Class Notes belongs to Uni Stu 4 at University of California - Irvine taught by Staff in Fall. Since its upload, it has received 76 views. For similar materials see /class/201929/uni-stu-4-university-of-california-irvine in University Studies at University of California - Irvine.




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Date Created: 09/12/15
WHITE DWARE LNSElRALLING ONTO MODERT T VMMASSIVE BL 7 s 1 I 39 Alberto Sesana PSU n k 39 Alberto Vecchio 7quot Mike Eracleous 7 Stginn Sigurdsson PSU ha I Drew 39Clausen PSU r 1 7 39 39 7 gt 7 Irvine 422009 1 1 Univers39kitys ti Eirining39ham PS U OUTLINE gt WD EMRIs why should we bother gt GW from WDs inspiralling onto MBHs gt Event rate estimates gt Electramagnetic signature gt SPH simulations work in progress WHAT IS AN EMRI An extreme mass ratio inspiral EMFiI is slow inspiral of a compact object WD NS BH onto a massive blac ho e may m Val f v 39 Different fr m standard tidal disrupti n E51335 reqL 39e different 2 more restrictive dynamical conditions event rate usually lower than standard tidal quotif 39V39 disruption rates UM vur M0 an m M i i ms in1 rod i sill Alwyn GW radiation EM signature from the inspiral Low redshift from the disruption cosmography Menou Haiman Kocsis 2008 Sesana Vecchio Eracleous amp Sigurdsson 2008 15 th A 33 39 2 k 1 WRzH 7 IV yIer 1 V71IID V Enljnml 7547 139 WW3 HWHJFJ I IIVI Tyr ao so 4o 20 1 NW yr 50 so 4o zo o ler 50 so 40 2o 50 so 4o 20 10 I I I I l1 l WWI 391 quot ummvur Ian1392 r I 10quot 10quot 01 10 001 lrequency Hz 1039 00 10 1 frequency Hz 10 10quot 001 01 10quot frequency Hz We consider a SNR threshold for detectability of 30 DMAxSNR1OO3OX1 MpC EVENT RATE ESTIMATION div l r dmd1mi Mm Assumption 1 BH density constant in the observable volume VOW m 43 7TDiIAX AL m Assumption 2 similar BHs reside in similar stellar environments 137 dn 1 dl dDIdm 7 d3 Assumption 3 disruption rate independent on the WD mass dFdnLLM FIM PWD G wr39ra T H erwel e DR WES Made Nalezyty amp Althaus 2004 x 7 I 70 as some disperzxon k Galaxy LF FaberJackson Mo quotquot if go Log 004 Hole Mn Aller amp Richstone 2002 However there are several uncertainties related to the ingredients shown in the previous slide gtThe FJ and the M6 relations are derived for massive galaxies gtThe shape of the galaxy LF taint end is debated mm Sample Popessa er al rzanoi RAssrsts sample Blanmneullznml SDSSheldaainple J r A mm min Trentham amp Tully 2002 Gonzalez et al 2006 c WD disrution rates er sinle BH 100000 1c06 M Msun Hopman preliminary results This is based 0h FekkerPianek eaieuiaijiehe Same Meh ieeerie ieehhieuee give rates i QC higher fer We EMRHS Freitag 2001 Detection rates Detectian rates yr 1 pessimistic aptimistic Schw no plunge 003 001 21 1 Schw plunge 015 003 3971 21 Kerr prograde 045 040 163 124 The ex siemce 039 a Subsiant a pru aft Qn 01 QWeccen39ir c iy EMFMs eg 1mm bmary breakwp CM giant emveUQpe Stripping mu d be decisive er a pas tive detedtim ELECTRO MAGNETIC COUNTERPATS oMOV99 incvt3D accretion expandng debris Xray emission debris photoionization Rantsiou et al 2008 Results for a CO 055MB WD 10 of the mass launched at the escape speed in a thin annulus expanding at the speed of sound 10 kms Calculation performed with CLOUDY Ferland et al 1998 Optical Lines 1 10 01 Intensity Relative to C II X1335 ltr 23 4 O O a n gt I 1 a m E m r E 5 5 1o 20 Time After Event days Time After Event days The ionizing radiation provided by the accreting source illuminates the debris producing a peculiar signature of recombination lines evolving in time L1036 ergs SIMULATING THE WD DISRUPTION gtModelling using two codes GADGET 2 Springel 2005 GRASP Laguna et al 1993 gtGADGET 2 modifications Add a BH particle introducing a PaczynskiWiita potential Aow accretion BHsink particle Add GW radiation term to the dynamics of the WD gtViscosity artificiay included in the form of an excess pressure oltsph tuned to match the viscous time of a SS disk with XSS01 151m 5139 iii i3sprlrlfj 1 Wu I ij lt 0 otherwise l 39 co 39 5 WD modeled as a politrope with F53 Partice distributed according to the LaneEmden equation solution reaxation to numerical equilibrium MWD055 Mg MBH104 Ma a105 M e02 i th834M 7 H r a V w W m W Ax H nw N Results dnamical evolution of the disk 2x104 4x104 6X104 8x104 1wa5 w 1H J CH eoofetion begin after 1 day Differential precession I quot quot WT 39l 3 LT 77 r L LJJL K J log Surface Density g cm 100 102 104 106 log Radius cm Next steps gtDetermine the observable properties radiation produced by the inner disk illuminates the material farther out assume an incident radiation SED similar to that observed in AGNs normalized to the accretion luminosity use CLOUDY to determine the ionization state and the emissivity of the gas gtncude a self consistent GW radiation treatment in terms of the SPH particles properties Centrella amp McMillan 1993 to describe the signature during the tidal disruption Summary gt WD EMRIs are potentially interesting source for astrophysics and cosmology gt Observable out to few hundred Mpc event rates in the range 001100yr gt Numbers sensitive to the BH spin and the typical WD eccentricity gt Peculiar EM signature Xray accretion flare optical and UV recombination lines WORK IN PROGRESS Better event rate estimation considering a reliable estimation of the faint end of the MBH mass function robust event rate scalings with MBH mass distribution of EMRls eccentricities Source localization for 39realistic39 event samples how well we can determine the WDMBH parameters if counterpart is faint how many 39targets39 in the error box Numerical simulation of WD disruption for a more realistic modeling of the counterpart how does accretion proceed which are the actual properties of the postdisruption debris Drew Clausen SOURCE LOCALIZATION Barack amp Cutler quote errorboxes of 27deg2 for 39standard39 EMRls We expect similar if not better localization for WD EMRIS Same SNR threshold errorbox 0c SNRZ Same LISA orbit modulation Similar mM2 ratio Additional modulation due to LISA response function Low redshift sources Just an handful of candidate galaxies inihe errorbox Counterpart probably much easier to find comparing to the MBHB merger case EARAME 1 ER SPACE QEEINI 1 log Tidal disruption radius of the WD 21 IBH13 th 77 mWD 171 is a fitting factor dependent on the WD EOS For a zero temperature 125 politrope the mass radius relation of the WD become t r 12 I A39ICH 25 mWD 33 lt gt lt MD mva Mon C Equating Rd to RLSO and RSCH for a Schwarzschild BH we obtain a 1 7 7 12 m 3 M x A 104er 1 M g 1 7 105MG Pquot am rise fall and upward sweeps the emergence of a global state Christopher ChaseDunn Institute for Research on WorldSystems and Department of Sociology University of California Riverside Thanks to E N Anderson and Peter Turchin for their contributions to ideas developed below Human Sciences and Complexity This is for an interactive teleconference on Human Sciences and Complexity a 4campus interdisciplinary project that includes scholars from UClrvine UCLA UCSan Diego and UCR It is based on research proposal that is being supported by the US National Science Foundation s program on Human Social Dynamics That proposal is available at The time of the interactive teleconference is from 2 to 305 on Friday October 14 and the UCR location Will be in Olmsted 1208 An earlier version of this lecture presented at the University of Victoria is available at Overall outline of the talk The comparative worldsystems perspective Small medium and large worldsystems Waves of network expansion and contraction rise of the Central System Hierarchy Formation The iteration Model Rise and fall and upward sweeps Semiperipheral marcher states Semiperipheral capitalist city states Modeling rise and fall and upward sweeps two systemic levels state and worldsystem From corewide empires to modern hegemons Waves of Colonization and Decolonization Global State Formation The comparative worldsystems perspective Systems of Societies as the Unit of Analysis for explaining Cultural evolution CorePeriphery Hierarchies Semiperipheral Development WorldSystems Small Medium and Large Semiperipheral Development Semiperipheral Regions are Most Often the Sites of Innovations in New Institutions and Technologies that lead to Upward Mobility andor Transform the Logic of Social Change Types of Semiperipheral Societies Semiperipheral Marcher Chiefdoms Patrick Kirch Semiperipheral Marcher States Semperipheral Capitalist City States Semiperipheral World Regions Europe Modern Hegemons Dutch British US Bounding premodern worldsystems Important interaction networks Waves of network expansion and contraction pulsation and eventual globalization Expansion of the central system and incorporation of other regional systems Polities bands tribes chiefdoms states empires 3am ECE R0 f C t 1 Ifasapntm an PMN T Y A i E d t e i E 539 c E 1751 m I 5 5 M Wgst p i1 1 i W e W 35 I 1 A 1 39 39 s E H c 5 i E i a Central pm 393 a g P u e f 1 n a 7 V 15 I I GrettaRoman a P 1 1 1 w 11 P a I 4 I Phase al 1quot a 12 E a i 4 3E L FlV P M g 11 pmquot H p s Medicml M M a P p M 3 11 Phasvn a N quotII quotquot1 M plum C cntrral PMM 3939393939 39 Waitem Phase 39 gf C39enfral PMN 3th 31 Phas e UFC 31131 PMN EDUCII CE Rise and Fall of large powerful polities with intermittent upsweeps Large Hegemons Without formal colonies Global State Hegml ns Formation with Colonial Empires CoreWide Empires Small States Chiefdoms I 3quot Time Iterative Causes of City and State Growth Urb an Growth f F Populatlon growth K State Expansion I4 Techniques of En qr nmg t l Power and i E Degradation Production 39 a I R H Population fi Pressure W CoreWide Empire VS Modern Hegemony Cure 2 o A 61 C EH13 lt OD I C RA 0 0 Q 0 0 O C ureiwide Empire Hegemunic Cure Slate Resistance and global polity formation WAVES OF COLONIZATION AND DECOLONIZATION SINCE THE 16TH CENTURY David P Henige Colonial Governors


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