Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... Normalised spectra of all central stars of planetary nebulae observed in the 075.D-0289 campaign ordered by increasing effective temperature from top to the bottom. ... The presence of a magnetic field in the central star may be the reason for this lack of symmetry, but observational works published in the literature have so far reported contradictory results. ... We determine the magnetic field from spectropolarimetric observations of ten central stars of planetary nebulae. ... Results. ...

... Jitter is usually very small in magnitude and random in effect, and is not expected to lead to systematic throughput changes. ... However, such a change should lead to an obvious decline in the strength of the comparison lines at one end of the spectrum relative to the other and not an overall decline in counts. No such effect is seen (the counts decline evenly from one end of the spectrum to the other). ... The value changes steadily, but not by enough to account for the changes in counts seen. ...

... Assured of a reliable method of solving the normal equations, we now consider the equations of condition. The observed magnitude m of a star at M air masses with true instrumental magnitude is modelled as ([ 10 ], [ 28 ]) . ... The effective extinction coefficient depends on the effective spectral gradient [ 29 ] of the star, for which we use some color index, affected by half the atmospheric reddening ([ 26 ], [ 10 ]): . ... Thus, for the B band of UBV, we use the (U-V) color. ...

Modelling the effects of FR II radio jets on the turbulent magnetic fields in the intra-cluster medium Mar tМn Huar te Espinosa , Mar tin Krause, Paul Alexander and Christian R. Kaiser. ... The plasma relaxes for a crossing time (118 Myr) and then we inject mass and x-momentum to a central control cylinder and experiment with the jets power: velociB µG RM maps We calculate RM= 812 dl rad m-2 from the jets' con3 tact discontinuity to the end of the domain along different viewing angles. ...

... Staff . ... Cosmic dust has been observed both in emission and extinction everywhere in our Galaxy as well as in many other galaxies. ... Dust grains are classically thought to form in the winds of Asymptotic Giant Branch (AGB) stars. However, nowadays there is increasing observational evidence for notable dust formation in Supernovae (SNe). ... Hence the observed dust mass of 0.7вИТ0.9M вКЩ in this source can be safely considered as indicative of the mass of freshly formed dust in SN ejecta. ...

Mikhail Medvedev (University of Kansas) HEA- 2007 , IKI, Moscow Missing baryons in inter-cluster gas Afshordi, et al, 2007 , astro-ph/0612700 35% +/- 8% Sample of 260 clusters WMAP SZ 3yr data Compared with 11 simulated clusters Assumed: Universal NFW profile Self-similarity Isothermal gas Possible explanations Observed stellar mass in galaxies: ~ 10% (Lin, et al, ... Simulations indicate that the effect is small (Dolag, et al, 2004) Can account for ~1-2% missing mass at most ...

... Note on Filters: . ... NGC 3351 is a mostly face-on late type spiral galaxy. It is marked by a bar like feature in its central regions and a strong inner ring of star formation. ... The galaxy was imaged through the A1,B1 and B5 filters over a total exposure time of 1936 seconds. ... The galaxy was imaged through the A1 filter for 450 seconds and the B1 filter for 1084 seconds. ... The galaxy was imaged through the A1 and V1 filters over a total exposure time of 1200 seconds. ...

... 1.Magnetic and magneto-elastic properties of heavy rare earth metals. ... High magnetic fields of 100 kOe and more were necessary to saturate the magnetization of havy rare earth metals. ... It was shown that the effective exchange field theory is sufficient for the description of the magnetic order in heavy rare earth metals and their compounds. ... The duality of the state of the magnetic carriers in the traditional 3d-magnetic materials. ... LHPP ISSP RAS © 2004 All rights reserved ...

... The concept of continuous solar wind developed in 1950's. First, Biermann (1951, 1957) observed comet tails as they passed close to the Sun , and explained the observed tail deflection by a continuous flux of protons from the Sun. Then Parker (1959) showed that the solar corona must expand, and called the outward streaming coronal gas 'solar wind'. ... The expanding solar wind drags also the solar magnetic field outward, forming what is called the interplanetary magnetic field (IMF) . ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... Parkes | ... Australia Telescope 20GHz Survey . ... Visiting Parkes radio telescope . Visiting Australia Telescope Compact Array . ... Parkes radio telescope webcam . ...

... The Search of a pulsar Once the dedispersed time series is obtained, a Fourier transformation is performed. ... 2 Binary parameters The orbit of a pulsar , as well as any object, in a binary system is determined in its geometrical characteristics, space displacement and syncronised in time by the following parameters : Semimajor axis Eccentricity Longitude of periastron Binary period Time of ascending node a e PB T0 True spin period and observed spin period The ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... Using the self-consistent 3D hydrodynamical code in Kobayashi et al. (2007) , we simulate the star formation and chemical enrichment history of the Universe. ... We also predict the rates of supernovae and gamma-ray bursts, and the properties of the host galaxies, which will be observed with the ANU's new SkyMapper telescope. ... Supernova feedback on galaxy formation. ... Feedback from active-galactic nuclei (AGN). ... COALA : Universe Galaxy AGN Star Planet ...

... Science Activities > PhD Thesis Topics offered by ESO Faculty Members > Thesis Topic: Star formation: probing magnetic fields and their spheres of influence . ... Observing with ESO Telescopes . ... ESO-MIDAS . ... ESO Data . ... Magnetic fields play a key role in the early formation of low mass stars, from regulating the initial collapse of the protostar, controlling accretion from large circumstellar disks and their evolution along the early main sequence. ... Return to list of thesis topics . ...

Next: Rapidly Rotating Stars Up: Discussion Previous: Relations . ... They attributed this to a mechanism which regulated stellar angular momentum through the accretion disk. ... While some of this may be due to sampling effects, the data seem to indicate that after a star loses its disk, either it continues its slow rotation for a period of time and then a rapid increase in rotation rate commences or spin up does not necessarily follow the loss of the disk. ...

The Effective Area of EPIC A comparison of MOS1, MOS2 and PN derived fluxes of 17 onaxis AGN observed between Revolutions 63 and 683 XMM EPIC MOS Steve Sembay ( sfs5@star.le.ac.uk ) MPE 04/05/06 The sample: Mixture of BL Lacs and Soft Excess AGN Orbit 63 75 82 94 95 95 96 107 161 192 277 301 451 621 655 ... See talk by Andy later 3c 273: Flux Comparison, 7.5"40" v 15"40" extraction radii pn MOS1 MOS2 XMM EPIC MOS Steve Sembay (sfs5@star.le.ac.uk) MPE 04/05/06 Problem with the psf? ...

Astronomy Discussion Forums . Forums: . Atm ћ Astrophotography ћ Blackholes ћ Blackholes2 ћ CCD ћ Celestron ћ Domes ћ Education . ... Observe Every Photon's Size Experiment . ... Post Message | ... Observe every photon's size experiment . 1.The slow process of the formation of the light diffraction pattern experiment . ... www.astronomy.net . ... Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

... Home Observing Central Park ? ... Beyond New York City . ... Observing Resources for Amateur Astronomers - Part 1: Beginning Observers . ... A History of the First Forty Years of the Amateur Astronomers Association . ... The AAA hosts solar observing in Central Park one Sunday afternoon€аeach month.€а WeтАЩre located right by Bethesda Terrace and Fountain , middle of Central Park, just north of 72nd street. ... 2016 Amateur Astronomers Association of New York Designed by Press Customizr Powered by ....

... Gravitational wave search provides insights into galaxy evolution and mergers . ... Is it possible that the gravitational effects attributed to dark matter could be caused by Jupiter-sized planets discovered orbiting other stars and also floating freely outside planetary systems? ... A large number of detected and undetected Jupiter-sized planets could not mimic the gravitational effects produced by dark matter for two reasons. ... Get instant access to subscriber content on Astronomy.com! ...