... Temp_2-10.)/100. ,0.9); # declare Cblu_2 = min( Temp_2 /30. , 1.0 ); #end # declare Color_1 = Cred_1, Cgrn_1, Cblu_1 ; # declare Color_2 = Cred_2, Cgrn_2, Cblu_2 ; # declare Spot_1 = Cred_1-0.1, Cgrn_1-0.1, Cblu_1-0.1 ; /* Ultimately need to define the surface of each star - in close binaries ... Roche equipotential */ /* Primary star (with spots) */ union { sphere { 0,1 texture { bozo scale 0.3 turbulence 0.9 texture_map { [ 0.0 ...

... Abstract: We present Monte Carlo radiative transfer simulations for spiral galaxies modelled as a stellar disk and a two-phase clumpy dust distribution. ... As a general result, clumpy models are less opaque than the corresponding homogeneous models. ... 0.00 0.15 0.50 0.1 0.5 1.0 2.0 5.0 10.0 0.25 X . ... We have also produced several homogeneous models, to compare to the clumpy models. ... Homogeneous and clumpy models with the same tauV have the same dust mass. ...

Skim Study in CM2 Minghui Lu University of Oregon 0 For Fully Inclusive b s group Notre Dame-Oregon-Pisa-SLAC-UCSC 0 Skim Study in CM2 ­ p.1 Outline Introduction 0 skim cuts 0 mass and energy spectrum The Comparison of 0 mass spectrum between SP5 MC and run1 data Preliminary 0 mass fit Outlook 0 Skim Study in ...

Next: Phenomenological Kick Velocity Up: Restrictions on the Scenario Previous: The COOC Criterion (Criterion . ... The results of testing and parameters without kick velocity are presented in the form of "topographical maps" (i.e. as isolines) of constant ``COOC'' criterion in the plane calculated separately for each of the binary species listed in Table  4 (Figures  16 - 20 ). The total COOC criterion calculated with equal weights is shown in Figure  21 . ...

... The properties of the dust grains (e.g., temperature and mass) can be derived from fitting far-IR SEDs (т??100 ЮМm). Only with SPIRE on Herschel has it been possible to get high spatial resolution at 200 to 500 ЮМm that is beyond the peak (~160 ЮМm) of dust emission in most galaxies. Aims: We investigate the differences in the fitted dust temperatures and masses determined using only 200 ЮМm data is for deriving these dust properties. ...

... I note that "Z" plays an important role in what the ALFA surveys will look for: . ... low Z . nearby low mass . ... Arecibo . ... ADBS (Arecibo Dual Beam Survey): Rosenberg & Schneider 2002. ... A few sources with unobvious optical counterparts. ... Coverage wins for volume, but if you do a shallow survey you are sampling only the nearby volume at low masses. ... So need artificial test sources to find completeness. ... Total volume within survey in which source could have been detected. ...

... Science . ... The goal is to bring together two communitities: the one working on star formation (mostly galactic) and the one working on the formation of young massive clusters (mostly extra-galactic). We will link galactic with extra-galactic work, optical/NIR techniques with sub-mm/mm/radio ones, the formation of stars with the one of massive star clusters - observations and theory. ... Coordinated by Marina Rejkuba (abstract) . ... How did star formation proceed in Globular Clusters? ...

... Астронет | ... Переменные Звезды | ... Микролинзирование . ... На протяжении последних нескольких лет в рамках проекта MACHO проводятся наблюдения микролинзирования звезд Большого Магелланова Облака - спутника нашей Галактики. Эффект микролинзирования заключается в гравитационной фокусировке света звезды массивным объектом, находящимся на луче зрения между звездой и наблюдателем. ... Согласно некоторым гипотезам, линзами могут являться реликтовые черные дыры или "нейтралинные звезды". ...

... Star Atlas . ... solar system . ... stars . ... Observe the Solar System . ... What factors determine if a massive star (say, 100 solar masses) forms instead of a Sun-like star? ... Stars of all masses form from dense clumps within exceptionally cold molecular clouds. ... Massive stars tend to form at the centers of high-mass reservoirs of gas. Get instant access to subscriber content on Astronomy.com! ... A gamma-ray burst hints that LIGO's double black holes started as one massive star . ...

... Phase light curves of binary model that consists of a primary component with mass M 1 and a secondary component with mass M 2 . ... The input parameters of the problem are the accretion rate onto the binary components ( ), the component mass ratio q = M 2 /M 1 , the orbital inclination to the line of sight , the eccentricity e, the rotation angle of the apsidal line relative to the observer , and the parameter c characterizing viscosity. ...

. Next: Eclipsing MSPs Up: Binary Neutron Stars Previous: Eccentricities of pulsar orbits . љ . During giant phase . During mass transfer the Roche-lobe is full . At the end of mass transfer . Hence, there is a link, . љ љ . Figure 48: . Jon Bell . Thu Dec 19 15:15:11 GMT 1996

Atm 2 ospheric time constant with MASS and FADE 0 A. Tokovinin CTIO, Chile Adaptive Optics time constant 0 = 0.314 r0/V0 = 0.057 6/5 [ Cn2(h) V5/3(h) dh MASS time constant: 0, MASS, Numerical simulation 1. Set turbulent layer strength (seeing) & sp. response Definition (1 rad phase difference between wavefronts at t= 0) ] 3/5 = 0.175 (2 DESI ) 3/5 ; 2 DESI = < [ IA(1ms)/ IA(3ms) ] >2 0, MASS, This is an approximation! ... The MASS method is approximate! ...

... Since the reddening found for the stars in Table 13 was small, no reddening correction was attempted. ... These diamonds indicate the positions of very low mass, 3 Myr old, objects from the work of Burrows et al. ... This optical V versus R - I scheme is a very powerful method of detecting very low mass (VLM) objects. ... Because of this, young brown dwarfs are intrinsically no more difficult to observe in the optical than low mass stars at the age of Orionis. ...

Magnetic Stars, 2011, pp. ... We discuss a recent detection of a strong, organized magnetic field in the bright, broad­line B2V star, HR 5907, using the ESPaDOnS spectropolarimeter on the CFHT as part of the Magnetism in Massive Stars (MiMeS) survey. ... 2010; Rivinius et al., 2010). ... From our longitudinal magnetic field measurements, we confirm this period, which we adopt as the rotational period of this star (see Fig. 1), making it the fastest rotating, non­degenerate magnetic massive star! ...

... The difference is that inertia is an inherent property of matter, while weight also depends on gravity. ... They use gravity, balancing its force on the astronaut's body against a calibrated spring or against the force of gravity on some calibrated weights. ... Using scales and the local force of gravity, one can determine gravitational mass; or else, one might dispense with gravity, like the astronauts aboard Skylab, sand measure the "inertial mass," and in principle they may differ. ...

Blackholes2 Forum Message . ... Photons Have Mass Also. ... Posted by Duane Eddy on October 21, 2004 14:38:35 UTC . Photons have zero rest mass, however when in motion they have a non-zero mass as does all forms of energy including charge. ... A charge is a standing wave. ... www.astronomy.net . About Astronomy Net | Advertise on Astronomy Net | ... Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

... 8, ``Celestial Mechanics'', 2002 Estimation of masses of some minor planets from observations of perturbed bodies O. M. Kochetova Institute of Applied Astronomy, St. Petersburg, Russia The most straightforward method of mass determination of minor planets is the dynamical one which uses the gravitational perturbations produced by minor planet in the motion of other bodies. ... The values of the masses of minor planets (15), (29) and (65) appear to be rather close in both papers. ...

... 1 7) 3 2008 p *.stm ( 4, 5, 6 ( 8, 9, 10 11). , , . 1 p 30 2009 MASS. 25 25 5 5 1 1 0.01 125 0.1 1 10 100 1000 10000 0.01 125 0.1 1 10 100 1000 10000 25 25 5 5 1 0.01 0.1 1 10 1 100 1000 10000 0.01 0.1 1 10 100 1000 10000 . 1: p 3 2008 30 2009 . A, : B, : C, : D. pmax p 2 = p N 1 2 (1 + ), N F (1 ) basetime, 1000, 1 1: A 2009 2007 1.017 1.023 1.027 B 1.023 1.023 1.038 C 1.022 1.015 1.028 D 1.014 1.018 1.039 N = Tb /Te . ... p, , 0.005. s2 B , A 0.005/FA + 0.005/FB . ... 2009 4 3 , 2 ., ...

Ultracompact dwarf galaxies (UCDs) are among the densest stellar systems in the Universe. With typical masses of 10^7 to 10^8 solar masses and half-mass radii between 10 to 100 pc they are more than a factor 1000 denser than dwarf galaxies of the same mass. They also show evidence for elevated mass-to-light ratios, which could be due to the presence of massive black holes or unusual stellar IMFs as a result of their extreme densities. ...

... We have examined the diversity of planets and planetary systems that arise from oligarchic growth and gas accretion onto massive cores, by means of N-body simulations combined with a sophisticated disc model. ... Slow planetary growth resulted from the relatively low mass of solids in the disc, and one consequence of this is that planets underwent limited orbital migration during the lifetime of the gas disc. ... Figure 1 shows an example of this migration behaviour in a single-planetin-a-disc run. ...