Essentials of Heat Transfer: Principles, Materials, and Applications, by Massoud Kaviany

brown dwarfs and exoplanets with precise light curves from programmes like the Kepler space telescope and CoRoT (Convection Rotation and Planetary Transits) have stimulated improvement in the techniques of modelling binary stars. The International Astronomical Union Symposium 282 (IAU S282, 2012, Slovakia), ‘From Interacting Binaries to Exoplanets: Essential Modeling Tools’ discusses the methods used in these related fields. The paper focuses include numerical algorithms for light curve modelling and for resolving stellar systems in imaging; the incorporation of physical details into computing codes; and the acquisition of high-quality data using a wide-field survey project, such as those associated with Kepler, LSST (the Large Synoptic Survey Telescope), and the Gaia space observatory. Traditional tools in the orbital study, including astrometry, the transit or eclipse method (which detects dips in a star’s brightness when planets crosses the line of sight), the radial velocity (Doppler) method (which detects wobbles in a star’s motion caused by the gravitational pull of orbiting planets), and the timing study of pulsars, are being improved to resolve interacting binaries and their accretion disks. The discovery of many exoplanets has also energized the field of stellar astrophysics, as more detailed atomic/ molecular data are being included in the spectral modeling of stellar atmosphere. In 2011, a huge pulsar-circling planet likely made of diamond (PSR J1719-1438 b) and the first circumbinary exoplanet (Kepler-16b) attracted the attention of the media. In 2012, the smallest exoplanet (KOI-961.03) with a size approximately that of Mars was found. Studies have shown that Jupiter-like planets are not more common than small, rocky planets, and terrestrial planets can exist in both close (separated by several AU) and wide binaries, whose light curves may appear similar to those of planets that revolve around a single star. Researchers are now refining many of the methods that are used to study the small–mass systems of brown dwarfs and exoplanets. However, computations concerning interacting stellar binaries and planet-star interaction using 3D radiation hydrodynamics and full non-LTE (local thermal equilibrium) spectral synthesis of stellar atmosphere are lacking. This book collects 160 articles each one to four pages long, including a question section as well as the transcripts of four panel discussions. The articles cover the following eight themes; (1) Multiwavelength photometry and spectroscopy of interacting binaries; (2) Observations and analysis of exoplanets and brown dwarfs; (3) Imaging techniques; (4) Modelling atmospheres of stars; (5) Synthetic light curves and velocity curves, synthetic spectra of binary stars and their accretion structures; (6) Analysis of spectra and light curves; (7) Formation and evolution of binary stars, brown dwarfs and planets; and (8) Hydrodynamic simulations of exoplanets and mass transfer in interacting binaries. Because many articles overlap each other in method or goal, these classifications do not clearly capture the research subjects. The page limit on each article may reduce the technical contents.