Old Glory, : March And Two - Step

https://digitalcommons.library.umaine.edu/mmb-ps/3094/thumbnail.jp

Beneath the Starry Flag : March and Two Step

https://digitalcommons.library.umaine.edu/mmb-ps/2322/thumbnail.jp

A Case for Employing Near-field Measurements to Detect Important Effluents from Nuclear Material Processing Operations

General discussion of effluents from nuclear material reprocessing operations and the opportunity to detect important effluents in the near-field domain

A 15.65 solar mass black hole in an eclipsing binary in the nearby spiral galaxy Messier 33

Stellar-mass black holes are discovered in X-ray emitting binary systems, where their mass can be determined from the dynamics of their companion stars. Models of stellar evolution have difficulty producing black holes in close binaries with masses >10 solar masses, which is consistent with the fact that the most massive stellar black holes known so all have masses within 1 sigma of 10 solar masses. Here we report a mass of 15.65 +/- 1.45 solar masses for the black hole in the recently discovered system M33 X-7, which is located in the nearby galaxy Messier 33 (M33) and is the only known black hole that is in an eclipsing binary. In order to produce such a massive black hole, the progenitor star must have retained much of its outer envelope until after helium fusion in the core was completed. On the other hand, in order for the black hole to be in its present 3.45 day orbit about its 70.0 +/- 6.9 solar mass companion, there must have been a ``common envelope'' phase of evolution in which a significant amount of mass was lost from the system. We find the common envelope phase could not have occured in M33 X-7 unless the amount of mass lost from the progenitor during its evolution was an order of magnitude less than what is usually assumed in evolutionary models of massive stars.Comment: To appear in Nature October 18, 2007. Four figures (one color figure degraded). Differs slightly from published version. Supplementary Information follows in a separate postin

Prospectus, February 16, 1978

STU-GO VACANCIES FILLED TODAY, TOMORROW; Trail is unopposed for presidential post; Ballje, Berry, Henze vie for veep\u27s job; Staff editorial: Should Parkland foot the bill for vets\u27 education?; Parkland College News in Brief: CHI helps you understand the doctor, SWAMP meets, Land lab has good season, SIU rep here today; Return of the Hilltoppers: Clambering up Mount Parkland -- \u27Because it was there!\u27; Treasury post draws two hopefuls; One running for secretary; Davis seeks PR position; Bundy unopposed in bid for student services post; Three candidates in race for convocations senator; Swanson pursuing office of day senator; Life spanning draws large crowd; Snow day melts extra study time; Will the big bands ever return?; Taped artist interviews at U of I; Toll free tax answers for Illinois residents; \u27Furry friends\u27 contest; Classifieds; State basketball tourney schedule; Women win 10th: Cobras take victory number 20; Long life program lists classes; Cherry Orchard opening is apple of Krannert\u27s eye; Bookworms invited to U of I; It\u27s tourney time; Women beat Kankakee, top .500; Bouncing Bob Basketball Bonanza: If you think LAST week was tough...; Bouncing Bob Basketball Bonanza; Men grab two more winshttps://spark.parkland.edu/prospectus_1978/1025/thumbnail.jp

Virtual Exploration of Safe Entry Zones in the Brainstem: Comprehensive Definition and Analysis of the Operative Approach

Background Detailed and accurate understanding of intrinsic brainstem anatomy and the inter-relationship between its internal tracts and nuclei and external landmarks is of paramount importance for safe and effective brainstem surgery. Using anatomical models can be an important step in sharpening such understanding. Objective To show the applicability of our developed virtual 3D model in depicting the safe entry zones (SEZs) to the brainstem. Methods Accurate 3D virtual models of brainstem elements were created using high-resolution magnetic resonance imaging and computed tomography to depict brainstem SEZs. Results All the described SEZs to different aspects of the brainstem were successfully depicted using our 3D virtual models. Conclusions The virtual models provide an immersive experience of brainstem anatomy, allowing users to understand the intricacies of the microdissection that is necessary to appropriately traverse the brainstem nuclei and tracts toward a particular target. The models provide an unparalleled learning environment for illustrating SEZs into the brainstem that can be used for training and research

Orexin receptors in GtoPdb v.2023.1

Orexin receptors (nomenclature as agreed by the NC-IUPHAR Subcommittee on Orexin receptors [43]) are activated by the endogenous polypeptides orexin-A and orexin-B (also known as hypocretin-1 and -2; 33 and 28 aa) derived from a common precursor, preproorexin or orexin precursor, by proteolytic cleavage and some typical peptide modifications [117]. Orexin signaling has been associated with regulation of sleep and wakefulness, reward and addiction, appetite and feeding, pain gating, stress response, anxiety and depression. Currently the orexin receptor ligands in clinical use are the dual orexin receptor antagonists suvorexant and lemborexant and daridorexant, which are used as hypnotics, and several dual and OX2-selective antagonists are under development. Multiple orexin agonists are in development for the treatment of narcolepsy and other sleep disorders. Orexin receptor 3D structures have been solved [146, 144, 55, 126, 47, 109, 7, 145]

Kepler eclipsing binary stars. VII. the catalogue of eclipsing binaries found in the entire Kepler data set

The primary Kepler Mission provided nearly continuous monitoring of ~200,000 objects with unprecedented photometric precision. We present the final catalog of eclipsing binary systems within the 105 deg2 Kepler field of view. This release incorporates the full extent of the data from the primary mission (Q0-Q17 Data Release). As a result, new systems have been added, additional false positives have been removed, ephemerides and principal parameters have been recomputed, classifications have been revised to rely on analytical models, and eclipse timing variations have been computed for each system. We identify several classes of systems including those that exhibit tertiary eclipse events, systems that show clear evidence of additional bodies, heartbeat systems, systems with changing eclipse depths, and systems exhibiting only one eclipse event over the duration of the mission. We have updated the period and galactic latitude distribution diagrams and included a catalog completeness evaluation. The total number of identified eclipsing and ellipsoidal binary systems in the Kepler field of view has increased to 2878, 1.3% of all observed Kepler targets

Masses, radii, and orbits of small Kepler planets : The transition from gaseous to rocky planets

We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O).Peer reviewedFinal Accepted Versio