Appendix B: The Effects of Thermal Changes on the "Absolute" Position of the Secondary . ... I will use the same nomenclature for the rod forces here as I used in Appendix A. In Appendix A, the axial force balance equation at the horizon was shown to be . ... The quantity that we really wish to derive is , where is the rod elongation at some initial epoch (i.e. when the rods were first tensioned) and where is the rod elongation at some later time after the rod temperatures had changed. ...

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Next: Disk Expansion and Up: The Epsilon Aurigae Previous: Vertical Structure of . ... We model disks with and without central holes and use a variety of midplane opacities and temperatures. ... The eclipse lightcurve was computed on a grid of 505 time steps separated by approximately 1.3 days, for a range of values of the disk scale height, , the inclination, i , and central hole radius, . The opacity parameter, approximately equal to the ``vertical'' optical depth of the disk, is: . ...

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• Calculation of Extinction from Optical Colors
• The AstroStat Slog Blog Archive Differential Emission Measure [Eqn]

... Science Users Information Future Facilities and Development E-ELT jump to navigation jump to content . ... Observing with ESO Telescopes . ... In December 2012 ESO Council fully approved the E-ELT Programme ( more , more , even more , still more ). ... In December 2014 ESO Council approved the construction of the E-ELT in two phases, and authorised spending on Phase 1 . ... 15 Jan 2012] Announcement of the E-ELT Workshop "Shaping E-ELT Science and Instrumentation" , 25 February 01 March 2013 . ...

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... It is reasonable to expect a priori that the evolution of events is strongly time dependent, so the star formation history in a galaxy is another important parameter. Therefore, by calculating the evolution of events after a -function like star formation burst,   one gets a Green function for any arbitrary star formation history. ... The source evolution in a galaxy with given star formation rate is thus calculated as . ...

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• Calculation of binary NS coalescence rates
• Discussion
• Why must a radiopulsar coupled with an optical star have high eccentricity?

PREDICTION MODE In prediction mode (indicated by '-z' on the command line, and sometimes called 'tz' mode), tempo calculates pulsar ephemerides over short periods of time (typically hours) in the form of a simple polynomial expansion. ... The time spans of the polynomial series are specified by giving a 'maximum hour angle' for observations along with a maximum time span over which a single series must be valid. Multiple series within a day are calculated when necessary. ...

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• imstat
• ATNF Media Release - December 1, 1998
• colden

... PRA 2010 U (1s)-U 91+ 92+ E=6.0 MeV/u Charge-transfer probability as a function of the impact parameter b I.I. Tupitsyn, Y.S. Kozhedub et al., ... PRA 2012 Ne(1s 2s 2p )-F8+(1s) 230 keV/u 2 2 6 The probability of Ne K-shell-vacancy production as a function of the impact parameter b I.I. Tupitsyn, Y.S. Kozhedub et al., PRA 2012 Ne(1s 2s 2p )-F8+(1s) 130 keV/u 2 2 6 The probability of Ne K-shell-vacancy production as a function of the impact parameter b I.I. Tupitsyn, Y.S. Kozhedub et al., ...

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• http://www.gao.spb.ru/russian/psas/ffk2013/tfiles/yerokhin_H2_FFK13.pdf
• http://www.gao.spb.ru/english/publ-s/viii-rfs/p125.pdf
• http://www.gao.spb.ru/english/publ-s/viii-rfs/p133.pdf

HST MOSES TITLE MISSION OPERATIONS, SYSTEMS ENGINEERING, & SOFTWARE PROGRAM ENGINEERING MEMORANDUM EM: MOSES-1268 DATE: December 2, 2005 Light Shield Baffle Temperature Predictions for One Gyro Science Operations Mode AUTHORS: /s/ Andrew M. Wong PHONE: 301-901-6172 ORGN: 46-12 REVISED: APPROVALS: J. Abel /s/ L. Dunham /s/ T. Cruz /s/ SUMMARY Thermal analysis was conducted to assess forward Sun Angles (SA) and their effect on HST light shield (LS) baffle temperatures. ...

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• Results and Discussions
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... Measurements Definition Sample Timestamp Definition : Time and date of measurement XML parameter : mtSampTime Windspeed Definition : 3 second rolling average of 250 millisecond samples XML parameter : mtWindspeed Units : MPH Raw Wind Direction Definition : 3 second rolling average of 250 millisecond samples XML parameter : mtRawWindDir Units : Degrees Adjusted Wind Direction ... XML parameter: mt60MinWindGustTime_2 Units: date and time ...

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• http://www.naic.edu/~phil/hardware/weatherstation/parameterDefinitions.pdf
• ALFA Calibration Diode Temperature (Full Band)

Some Effects of Earthquakes, Temperature, Wind Stor ms and Barometric Pressure on the Inter ferometer at Hanford Robert Schofield Masahiro Ito Rauha Rahkola Evan Mauceli Ray Frey David Strom Jim Brau University of Oregon Some Concerns With Low Frequency Influences · Loss of lock · Need for increased servo loop gain · May eat up actuator range · Possible increased background in the LIGO frequency band · Possible modulation of noise in the LIGO band Guralp ...

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• Current Weather Conditions
• Lecture XVII.
• Astronomy HyperText Book: Fusion Sequences in Stars

Observed maximum rotation velocity uncorrected for inclination effect. This quantity is calculated from 21-cm line widths at different levels and/or rotation curves (generally in H_alpha). ... These data are characterized by some secondary parameters: telescope, velocity resolution, level of the 21-cm line width and bibliographic reference. ... we start from a standard sample (a set of measurements giving a large and homogeneous sample). ... HyperLeda . ...

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• Documentation: LEDA: parameter: vrot
• Eddington's Temperature of Space
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This document explains values, tables and other matters on solar physics computing pages. ... is040423.ete : SAHA-S tables, interpolation values: T, rho, X. Z is fixed at 0.02. See reference above. opal2005.etf : OPAL EOS, interpolation values: T, rho, X, Z. Downloaded from OPAL site , marked there as "2005", seems to be unpublished. opal2001.etf : OPAL EOS, interpolation values: T, rho, X, Z. Rogers F.J., Nayfonov A. Astrophys. ... The following values can be calculated: . ... dimensionless . ...

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... We have carried out quantitative analyses of three very low surface gravity extreme helium stars with very similar spectra. ... In addition to the high carbon and nitrogen abundances usually seen in extreme helium stars, two of the programme stars have extremely high oxygen abundances, comparable with or greater than their carbon abundances. Based on observations obtained at the European Southern Observatory, La Silla, Chile. ...