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Ultimate Star Wars
Because numerous aliens, droids, starships, weapons and locations are never identified on screen, it can be quite a challenge for fans to learn more about specific subjects. This unique compendium features a wealth of images and information about many characters, creatures, vehicles, devices, and locates. Each is presented in chronological order according to its first appearance in the Star War movies, The Clone Wars, Rebels, Resistance, and other official lore. -- Adapted from Introduction.
Book
POSYDON: A General-purpose Population Synthesis Code with Detailed Binary-evolution Simulations
Most massive stars are members of a binary or a higher-order stellar system, where the presence of a binary companion can decisively alter their evolution via binary interactions. Interacting binaries are also important astrophysical laboratories for the study of compact objects. Binary population synthesis studies have been used extensively over the last two decades to interpret observations of compact-object binaries and to decipher the physical processes that lead to their formation. Here, we present POSYDON, a novel, publicly available, binary population synthesis code that incorporates full stellar structure and binary-evolution modeling, using the MESA code, throughout the whole evolution of the binaries. The use of POSYDON enables the self-consistent treatment of physical processes in stellar and binary evolution, including: realistic mass-transfer calculations and assessment of stability, internal angular-momentum transport and tides, stellar core sizes, mass-transfer rates, and orbital periods. This paper describes the detailed methodology and implementation of POSYDON, including the assumed physics of stellar and binary evolution, the extensive grids of detailed single- and binary-star models, the postprocessing, classification, and interpolation methods we developed for use with the grids, and the treatment of evolutionary phases that are not based on precalculated grids. The first version of POSYDON targets binaries with massive primary stars (potential progenitors of neutron stars or black holes) at solar metallicity.
Journal Article
How Star Wars conquered the universe : the past, present, and future of a multibillion dollar franchise
Traces the history of the film series from the difficult creation of the original film to the preparations for a new trilogy, providing portraits of the people who labored behind the scenes to turn George Lucas' idea into a legend.
Book
Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Massive stars (∼8–25 M ⊙) stripped of their hydrogen-rich envelopes via binary interaction are thought to be the main progenitors for merging neutron stars and stripped-envelope supernovae. We recently presented the discovery of the first set of such stripped stars in a companion paper. Here, we fit the spectra of 10 stars with new atmosphere models in order to constrain their stellar properties precisely. We find that the stellar properties align well with the theoretical expectations from binary evolution models for helium-core burning envelope-stripped stars. The fits confirm that the stars have high effective temperatures (T eff ∼ 50–100 kK), high surface gravities ( logg∼ 5), and hydrogen-poor/helium-rich surfaces (X H,surf ∼ 0–0.4) while showing for the first time a range of bolometric luminosities (103–105 L ⊙), small radii (∼0.5–1 R ⊙), and low Eddington factors (Γ e ∼ 0.006–0.4). Using these properties, we derive intermediate current masses (∼1–8 M ⊙), which suggest that their progenitors were massive stars (∼5–25 M ⊙) and that a subset will reach core-collapse, leaving behind neutron stars or black holes. Using the model fits, we also estimate the emission rates of ionizing photons for these stars, which agree well with previous model expectations. Further, by computing models for a range of mass-loss rates, we find that the stellar winds are weaker than predicted by any existing scheme ( Ṁwind≲10−9 M ⊙ yr−1). The properties of this first sample of intermediate-mass helium stars suggest they both contain progenitors of type Ib and IIb supernovae, and provide important benchmarks for binary evolution and population synthesis models.
Journal Article
Star wars : on the front lines
\"From the Clone Wars and the Rebellion to the clashes with the First Order, the galaxy is defined by war. Star Wars: On the Front Lines chronicles the tactics, weapons, and armor used in pivotal battles along with acts of valor achieved during the campaign. By focusing on elements of the battles that occurred \"off screen,\" this collection brings the struggles faced by ground soldiers and starfighter pilots to life like never before, placing the reader on the battlelines\"--Amazon.
Book
Classical OBe Stars as Post-supernova Runaways: Confirming Binary Origins
Massive binaries play an important role in fields ranging from gravitational-wave astronomy to stellar evolution. We provide several lines of evidence that classical OBe stars in the Small Magellanic Cloud (SMC) obtain their rapid rotation from mass and angular momentum transfer in massive binaries, which predicts that the subsequent supernovae should often eject OBe stars into the field. We find that (1) OBe stars have a higher field frequency than OB stars; (2) our cumulative distribution function (CDF) of stellar distances from O stars shows that OBe stars are indeed much more isolated than ordinary OB stars of corresponding spectral types; (3) the CDFs of OBe stars approach that of high-mass X-ray binaries (HMXBs), which are confirmed post-supernova objects; and (4) Oe stars are as isolated from clusters as Be stars, implying that their final masses are relatively independent of their initial masses, consistent with major mass transfer. Lastly, we also find that the spatial distribution of supergiant OBe stars differs from that of classical OBe stars, consistent with the different mechanisms responsible for their emission-line spectra.
Journal Article
Star wars character encyclopedia
\"Meet more than 200 Star Wars characters. The definitive guide to the heroes, villains, aliens, and droids fro the Star Wars galaxy features detailed character profiles, little-known facts, and amazing movie images. Fully revised and updated.\"--Page 4 of cover.
Book
Massive Star Cluster Formation with Binaries. I. Evolution of Binary Populations
We study the evolution of populations of binary stars within massive cluster-forming regions. We simulate the formation of young massive star clusters within giant molecular clouds with masses ranging from 2 × 104 to 3.2 × 105 M ⊙. We use Torch, which couples stellar dynamics, magnetohydrodynamics, star and binary formation, stellar evolution, and stellar feedback through the Amuse framework. We find that the binary fraction decreases during cluster formation at all molecular cloud masses. The binaries’ orbital properties also change, with stronger and quicker changes in denser, more massive clouds. Most of the changes we see can be attributed to the disruption of binaries wider than 100 au, although the close binary fraction also decreases in the densest cluster-forming region. The binary fraction for O stars remains above 90%, but exchanges and dynamical hardening are ubiquitous, indicating that O stars undergo frequent few-body interactions early during the cluster formation process. Changes to the populations of binaries are a by-product of hierarchical cluster assembly: most changes to the binary population take place when the star formation rate is high, and there are frequent mergers between subclusters in the cluster-forming region. A universal primordial binary distribution based on observed inner companions in the Galactic field is consistent with the binary populations of young clusters with resolved stellar populations, and the scatter between clusters of similar masses could be explained by differences in their formation history.
Journal Article
Star Wars year by year : a visual history
The definitive history of \"Star Wars\" chronicling four decades of the world of \"Star Wars\"; decade by decade, year-by-year, month-by-month. Everything is covered, from the influences and creation of all six \"Star Wars\" movies, to the toys, books and video games that have shaped the \"Star Wars\" dynasty. The month-by-month format is brought to life by images from the movies, TV series, comic books and more.
Book
Born to Be Wide: The Distribution of Wide Binaries in the Field and Soft Binaries in Clusters
Most stars, binaries, and higher-multiplicity systems are thought to form in stellar clusters and associations that later dissociate. Very wide binaries can be easily disrupted in clusters due to dynamical evaporation (soft binaries) and/or tidal disruption by the gravitational potential of the cluster. Nevertheless, wide binaries are quite frequent in the field, where they can sometimes play a key role in the formation of compact binaries and serve as tools to study key physical processes. Here we use analytic tools to study the dynamical formation of soft binaries in clusters and their survival as field binaries following cluster dispersion. We derive the expected properties of very wide binaries both in clusters and in the field. We analytically derive their detailed distributions, including the wide binary fraction as a function of mass in different cluster environments, binary mass functions and mass ratios, and the distribution of their orbital properties. We show that our calculations agree well in most aspects with the results of N-body simulations but show some different binary fraction dependence on the cluster mass. We find that the overall fraction of wide binaries scales as ∝N⋆−1 , where N ⋆ is the size of the cluster, even for non-equal-mass stars. More massive stars are more likely to capture wide companions, with most stars above 5 M ⊙ likely to capture at least one stellar companion, and formation of triples is found to be frequent.
Journal Article