Results 11 to 20 of about 1,661,126 (377)

The Scintillation of Stars [PDF]

open access: bronzeNature, 1950
IN a recent communication in Nature1, Dr. A. H. R. Goldie has suggested that the scintillation of stars may be associated with waves at an interface between two currents of air which have a difference of temperature of the order of 5–7° F. “Such waves,” he writes, “should not uncommonly have an amplitude of the order of up to 500–1,000 ft.
A. H. R. Goldie
openalex   +6 more sources

The single star path to Be stars [PDF]

open access: yesAstronomy & Astrophysics, 2020
Context. Be stars are rapidly rotating B main sequence stars that show line emission due to an outflowing disc. By studying the evolution of rotating single star models, we can assess their contribution to the observed Be star populations. Aims. We identify the main effects that cause single stars to approach critical rotation as functions of initial ...
Ben Hastings, Chen Wang, Norbert Langer
openaire   +3 more sources

A Phenomenographic Study of Adolescents’ Conceptions of Health Information Appraisal as a Critical Component of Adolescent Health Literacy

open access: yesActa Paedagogica Vilnensia, 2020
This paper reports on a health literacy study that explored adolescents’ conceptualizations of health information appraisal as a social practice in Latvia. The study was guided by phenomenography, a qualitative research approach used to describe people’s
Inese Stars, Zanda Rubene
doaj   +1 more source

Evidence for quark-matter cores in massive neutron stars [PDF]

open access: yesNature Physics, 2019
The theory governing the strong nuclear force—quantum chromodynamics—predicts that at sufficiently high energy densities, hadronic nuclear matter undergoes a deconfinement transition to a new phase of quarks and gluons1.
Eemeli Annala   +4 more
semanticscholar   +1 more source

INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS [PDF]

open access: yes, 2013
We present an analysis of the intrinsic colors and temperatures of 5–30 Myr old pre-main-sequence (pre-MS) stars using the F0- through M9-type members of nearby, negligibly reddened groups: the η Cha cluster, the TW Hydra Association, the β Pic Moving ...
M. Pecaut, E. Mamajek
semanticscholar   +1 more source

Full-thickness Skin Micro-columns within a Dermal Matrix: A Novel Method for “Donor-free” Skin Replacement

open access: yesPlastic and Reconstructive Surgery, Global Open, 2020
Summary:. Split-thickness skin graft has been the standard in the coverage of large full-thickness skin defects. However, donor sites can be associated with significant pain and scarring.
Laura Cooper, MD   +3 more
doaj   +1 more source

Measuring neuropsychiatric symptoms in patients with early cognitive decline using speech analysis

open access: yesEuropean Psychiatry, 2021
Background Certain neuropsychiatric symptoms (NPS), namely apathy, depression, and anxiety demonstrated great value in predicting dementia progression, representing eventually an opportunity window for timely diagnosis and treatment.
Alexandra König   +6 more
doaj   +1 more source

Tree and 1-loop fundamental BCJ relations from soft theorems

open access: yesEuropean Physical Journal C: Particles and Fields, 2023
We provide a new derivation of the fundamental BCJ relation among double-color-ordered tree amplitudes of bi-adjoint scalar theory, based on the leading soft theorem for external scalars. Then, we generalize the fundamental BCJ relation to 1-loop Feynman
Fang-Stars Wei, Kang Zhou
doaj   +1 more source

Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817. [PDF]

open access: yesPhysical Review Letters, 2018
We use gravitational-wave observations of the binary neutron star merger GW170817 to explore the tidal deformabilities and radii of neutron stars.
S. De   +5 more
semanticscholar   +1 more source

Protoneutron stars and neutron stars [PDF]

open access: yesInternational Astronomical Union Colloquium, 2000
Abstract We find constraints on minimum and maximum mass of ordinary neutron stars imposed by their early evolution (protoneutron star stage). We calculate models of protoneutron stars using a realistic standard equation of state of hot, dense matter valid for both supranuclear and subnuclear densities.
D. Gondek-Rosinska   +2 more
openaire   +3 more sources

Home - About - Disclaimer - Privacy