'Binary systems' presentation slideshows

CHEM 212

CHEM 212. Chapter 5 Phases and Solutions. Dr. A. Al-Saadi. Things to be Covered in This Chapter. Substances can exist in more than one phase. Introduction to phases, phase recognitions and equilibrium between phases. Clapeyron equation and Clausius-Clapeyron equation for phase changes.

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Tutorial/HW Week #7 WWWR Chapters 24-25 ID Chapter 14

Tutorial #7 WWWR# 24.1, 24.12, 24.13, 24.15(d), 24.22. To be discussed on March 11, 2014. By either volunteer or class list. Tutorial/HW Week #7 WWWR Chapters 24-25 ID Chapter 14. Molecular Mass Transfer. Molecular diffusion Mass transfer law components: Molecular concentration:

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IR Interferometry of stellar sources: Lessons learned and perspectives

IR Interferometry of stellar sources: Lessons learned and perspectives. A. Richichi (ESO Garching). LBT 2002 Bertinoro (Forli'), 7-9 October 2002. (Michelson) Interferometry at work - I. So now what?. (Michelson) Interferometry at work - II. Interf. Fringes. Single Telescope. Objects.

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CS231: Computer Architecture I

CS231: Computer Architecture I. Friday, February 1, 2008. Announcements. Homework 1 is due Monday @ 5:00pm Turn in to TA Office 0212 SC (In Basement) Slide it under the door! NOT Outside in bins!!! Late homeworks accepted with penalty By Tuesday @ 5:00pm: -10%

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Binary Black Holes and Gravitational Waves

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Neutron Stars 2: Phenomenology

Neutron Stars 2: Phenomenology. Chandra x-ray images of the PWNs surrounding the ( A ) Crab and ( B ) Vela pulsars. [Credit: NASA/CXC/Smithsonian Astrophysical Observatory, NASA/Pennsylvania State University, and G. Pavlov] . Andreas Reisenegger ESO Visiting Scientist

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S-72.1140 Transmission Methods in Telecommunication Systems (5 cr)

S-72.1140 Transmission Methods in Telecommunication Systems (5 cr). Digital Bandpass Transmission. Digital Bandpass Transmission. CW detection techniques Coherent Non-coherent Differentially coherent Examples of coherent and non-coherent detection error rate analysis (OOK)

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Observations of BSS in

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Neutron Stars 4: Magnetism

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t he brightest stars do not live alone

t he brightest stars do not live alone. B ackground Design E. Buunk / S.E. de Mink, HST image: NASA Paresce. Selma E. de Mink Hubble Science Briefing , February 7, 2013 Hubble Fellow at Space Telescope Science Institute / Johns Hopkins University. t he brightest stars .

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Gravitational waves from short Gamma-Ray Bursts Dafne Guetta (Rome Obs.)

Gravitational waves from short Gamma-Ray Bursts Dafne Guetta (Rome Obs.) In collaboration with Luigi Stella. DNSs sources of Short GRBSs.

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Measuring Stars

Measuring Stars. Easy. Hard. Binary Stars. What We Want to Know. Brightness Temperature Composition Distance Luminosity Size (Radius) Mass. l peak T = 2900 K ?? m. Spectrum tells you composition. ( M + m ) P 2 = a 3. Spectrum also tells you much more. Luminosity and Brightness.

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Gravitational Waves: a new window to the Universe

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VIRGO-bars joint data analysis

VIRGO-bars joint data analysis. Francesco Salemi for the VIRGO-bars Collaboration. Summary. INTRO Target Signals Sensitivity Curves Exchanged data MDC injections Time errors 2-fold Coincidence Analysis Optimization of the thresholds Background & Efficiency Statistical Analysis

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Fresnel Diffractive Arrays Imagery

Fresnel Diffractive Arrays Imagery. Sky observation Targets. Presented by Truswin Raksasataya. Agenda. Sky validation and its objectives FDAI Gen II configurations FDAI Gen II Estimation First Results Future Targets. Sky observation for Prototype II.

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Spectral lines

Spectral lines. Photon energy Atomic structure Spectral lines Elements in stars Masses of stars Mass-luminosity relation Reading: sections 16.5, 16.7, 6.2. Photon energy. Up to now, we have been discussing the wavelength of light as determining it color

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Multiple Star Formation at the Bottom of the IMF

Multiple Star Formation at the Bottom of the IMF. Adam L. Kraus February 1, 2007. Background: Field Binaries. Solar-type binaries : High binary frequency Large separations Low companion masses. Brown dwarf binaries : Low binary frequency Small separations Near-equal masses.

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7. Excess Gibbs Energy Models

7. Excess Gibbs Energy Models. Practicing engineers find most of the liquid-phase information needed for equilibrium calculations in the form of excess Gibbs Energy models. These models: reduce vast quantities of experimental data into a few empirical parameters,

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Measuring the Spin-Orbit Alignments of Transiting Exoplanetary Systems: The Case for TrES-1

The Rossiter-McLaughlin Effect What can we learn from this effect?. Formation Models of Close-in Planets How have they migrated to their current position?. Planet migration mechanisms and outcomes: Disk-Planet interaction e.g., Lin et al. 1996

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