Shock Models

2009 ◽  
pp. 59-76 ◽  
Author(s):  
Allan Gut ◽  
Jürg Hüsler
Keyword(s):  
Shock Models

A new class of bivariate Lindley distributions based on stress and shock models and some of their reliability properties

2021 ◽  
pp. 107528
Author(s):  
Ricardo P. Oliveira ◽  
Jorge A. Achcar ◽  
Josmar Mazucheli ◽  
Wesley Bertoli
Keyword(s):  
New Class ◽  
Shock Models

scholarly journals sGCα1β1 attenuates cardiac dysfunction and mortality in murine inflammatory shock models

2009 ◽  
Vol 9 (S1) ◽  
Author(s):  
Emmanuel S Buys ◽  
Anje Cauwels ◽  
Michael J Raher ◽  
Jonathan J Passeri ◽  
Ion Hobai ◽  
...  
Keyword(s):  
Cardiac Dysfunction ◽  
Shock Models

scholarly journals Shock models under a Markovian arrival process

2009 ◽  
Vol 50 (5-6) ◽  
pp. 879-884 ◽  
Author(s):  
Rafael Pérez-Ocón ◽  
Maria del Carmen Segovia
Keyword(s):  
Markovian Arrival Process ◽  
Arrival Process ◽  
Shock Models

scholarly journals Multivariate reliability modelling based on dependent dynamic shock models

2017 ◽  
Vol 51 ◽  
pp. 199-216 ◽  
Author(s):  
Ji Hwan Cha ◽  
F.G. Badía
Keyword(s):  
Reliability Modelling ◽  
Shock Models

scholarly journals Far-IR Spectrophotometry of HH Flows with the ISO Long-Wavelength Spectrometer

1997 ◽  
Vol 182 ◽  
pp. 111-120
Author(s):  
R. Liseau ◽  
T. Giannini ◽  
B. Nisini ◽  
P. Saraceno ◽  
L. Spinoglio ◽  
...  
Keyword(s):  
Mass Loss ◽  
Line Emission ◽  
Young Stellar Objects ◽  
Stellar Objects ◽  
Star Forming ◽  
Star Forming Regions ◽  
Shock Models ◽  
Ir Spectrophotometry ◽  
Hh Objects ◽  
Loss Rates

Full Iso-Lws spectral scans between about 45 to 190 μm of 17 individual HH objects in 7 star forming regions have revealed essentially only [O I] 63 μm line emission, implying that the Fircooling of these objects is totally dominated by this line alone. In this case, J-shock models can be used to determine the mass loss rates of the HH exciting sources. These mass loss rates are in reasonably good agreement with those estimated for the accompanying CO flows, providing first observational evidence that HH and molecular flows are driven by the same agent. The Lmech – Lbol relation, based on our results with the Lws, implies that young stellar objects of lower mass are loosing mass at relatively higher rates than their more massive counterparts.

scholarly journals A generalized class of correlated run shock models

2018 ◽  
Vol 6 (1) ◽  
pp. 131-138 ◽  
Author(s):  
Femin Yalcin ◽  
Serkan Eryilmaz ◽  
Ali Riza Bozbulut
Keyword(s):  
Stopping Time ◽  
Random Variables ◽  
Random Variable ◽  
Phase Type Distribution ◽  
Type Distribution ◽  
Shock Models ◽  
Phase Type ◽  
Over Time

AbstractIn this paper, a generalized class of run shock models associated with a bivariate sequence {(Xi, Yi)}i≥1 of correlated random variables is defined and studied. For a system that is subject to shocks of random magnitudes X1, X2, ... over time, let the random variables Y1, Y2, ... denote times between arrivals of successive shocks. The lifetime of the system under this class is defined through a compound random variable T = ∑Nt=1 Yt , where N is a stopping time for the sequence {Xi}i≤1 and represents the number of shocks that causes failure of the system. Another random variable of interest is the maximum shock size up to N, i.e. M = max {Xi, 1≤i≤ N}. Distributions of T and M are investigated when N has a phase-type distribution.

scholarly journals Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7

2018 ◽  
Vol 609 ◽  
pp. A40 ◽  
Author(s):  
B. Epinat ◽  
T. Contini ◽  
H. Finley ◽  
L. A. Boogaard ◽  
A. Guérou ◽  
...  
Keyword(s):  
Physical Properties ◽  
High Velocity ◽  
Active Galactic Nucleus ◽  
Dense Region ◽  
Tidal Forces ◽  
Shock Models ◽  
The Galaxy ◽  
Group Members ◽  
Low Mass ◽  
Massive Galaxy

We report the discovery of a 104 kpc2 gaseous structure detected in [O ii]λλ3727, 3729 in an over-dense region of the COSMOS-Gr30 galaxy group at z ~ 0.725 with deep MUSE Guaranteed Time Observations. We estimate the total amount of diffuse ionised gas to be of the order of (~5 ± 3) × 1010 M⊙ and explore its physical properties to understand its origin and the source(s) of the ionisation. The MUSE data allow the identification of a dozen group members that are embedded in this structure through emission and absorption lines. We extracted spectra from small apertures defined for both the diffuse ionised gas and the galaxies. We investigated the kinematics and ionisation properties of the various galaxies and extended gas regions through line diagnostics (R23, O32, and [O iii]/Hβ) that are available within the MUSE wavelength range. We compared these diagnostics to photo-ionisation models and shock models. The structure is divided into two kinematically distinct sub-structures. The most extended sub-structure of ionised gas is likely rotating around a massive galaxy and displays filamentary patterns that link some galaxies. The second sub-structure links another massive galaxy that hosts an active galactic nucleus (AGN) to a low-mass galaxy, but it also extends orthogonally to the AGN host disc over ~ 35 kpc. This extent is likely ionised by the AGN itself. The location of small diffuse regions in the R23 vs. O32 diagram is compatible with photo-ionisation. However, the location of three of these regions in this diagram (low O32, high R23) can also be explained by shocks, which is supported by their high velocity dispersions. One edge-on galaxy shares the same properties and may be a source of shocks. Regardless of the hypothesis, the extended gas seems to be non-primordial. We favour a scenario where the gas has been extracted from galaxies by tidal forces and AGN triggered by interactions between at least the two sub-structures.

The “Line of Death” for the synchrotron shock models: Confronting the data

1998 ◽  
Author(s):  
R. D. Preece ◽  
M. S. Briggs ◽  
R. S. Mallozzi ◽  
G. N. Pendleton ◽  
W. S. Paciesas ◽  
...  
Keyword(s):  
Shock Models
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