Results 1 to 10 of about 117,260 (302)
Similar Simulation Test on Deformation Characteristics of Overlying Rock Developed by Instability of Strip Coal Pillar [PDF]
Shock and Vibration, 2022 In order to protect surface buildings and maximize the recovery of coal resources, there are a large number of strip coal pillars and unfilled goafs left in strip mining areas in China.
Yong Liu +3 more
doaj +2 more sources
Re-defining the Empirical ZZ Ceti Instability Strip [PDF]
The Astrophysical Journal, 2004 We use the new ZZ Ceti stars (hydrogen atmosphere white dwarf variables; DAVs) discovered within the Sloan Digital Sky Survey (Mukadam et al. 2004) to re-define the empirical ZZ Ceti instability strip.
A. F. M. Costa +8 more
core +4 more sources
Comparative seismology of pre- and main sequence stars in the instability strip [PDF]
, 2001 Pulsational properties of 1.8 M$_{\odot}$ stellar models covering the latest stages of contraction toward the main sequence up to early hydrogen burning phases are investigated by means of linear nonadiabatic analyses.
M. Suran +4 more
openalex +4 more sources
The Instability Strip for Pre--Main-Sequence Stars [PDF]
The Astrophysical Journal, 1998 We investigate the pulsational properties of Pre--Main-Sequence (PMS) stars by means of linear and nonlinear calculations. The equilibrium models were taken from models evolved from the protostellar birthline to the ZAMS for masses in the range 1 to 4 ...
Baade D. +9 more
core +5 more sources
Dwarf nova EZ Lyncis second visit to instability strip [PDF]
Publications of the Astronomical Society of Japan, 2014 Abstract The analysis of 14 periodograms of EZ Lyn for data spaced over 565 d in 2012–2014 (2–3.5 yr after the 2010 outburst) yielded the existence of a stable signal around 100 cycles/day (c/d) and three signals around 310 c/d, 338 c/d, and 368 c/d (the corresponding periods are 864 s, 279 s, 256 s, and 235 s).
Elena P. Pavlenko +7 more
openalex +5 more sources
Instability strip for pre-main-sequence stars [PDF]
Communications in Asteroseismology, 2007 We apply the Time Dependent Convection (TDC) treatment presented in Grigahcene et al. (2005) to the study of Pre-main sequence pulsating stars. The stabilization of the p-modes at the red edge of the Instability Strip (IS) is obtained by our models. The theoretical IS obtained with Mixing Length (ML) parameter α =1.8 is compared to observations and a ...
A. Grigahcène
openalex +3 more sources
The First Theoretical γ Doradus Instability Strip [PDF]
International Astronomical Union Colloquium, 2004 AbstractWe present the first theoretical γ Doradus instability strip. We find that our model instability strip agrees very well with the previously established, observationally based, instability strip of Handler & Shobbrook (2002). We stress, as in Guzik et al. (2000), that the convection zone depth plays the major role in the determination of our
A. B. Kaye +2 more
openalex +2 more sources
A New Instability Strip for Hot Degenerates [PDF]
International Astronomical Union Colloquium, 1980 A completely new kind of variable star has recently been discovered (McGraw, et. al. 1979). Designated as PG1159-035 (hereafter PG) this star is distinguished not only by the complete lack of hydrogen in its spectrum but also by an effective temperature that exceeds 8 × 104 K (McGraw, private communication).
S. Starrfield, A. N. Cox, S. W. Hodson
openalex +3 more sources
The Instability Strip of M3 [PDF]
International Astronomical Union Colloquium, 2000 We present new multicolour CCD photometry of the central part of the globular cluster M3, mapping the precise position of ~120 RR Lyrae stars (RRab, RRd, RRc) on the horizontal branch (HB). The location of the double-mode variables (RRd) is in perfect agreement with recent theoretical results.
G. Á. Bakos, J. Jurcsik
+5 more sources
A search for non-pulsating, chemically normal stars in the δ Scuti instability strip using Kepler data [PDF]
, 2015 We identify stars in the δ Sct instability strip that do not pulsate in p modes at the 50-μmag limit, using Kepler data. Spectral classification and abundance analyses from high-resolution spectroscopy allow us to identify chemically peculiar stars, in ...
Simon J. Murphy +4 more
openalex +6 more sources