Improved coastal hydrodynamic model offers insight into surface and groundwater flow and restoration objectives in Biscayne Bay, Florida, USA

2015 ◽  
Vol 91 (4) ◽  
pp. 433-454 ◽  
Author(s):  
Erik Stabenau ◽  
Amy Renshaw ◽  
Jiangang Luo ◽  
Edward Kearns ◽  
John D Wang
2011 ◽  
Vol 15 (suppl. 1) ◽  
pp. 131-135 ◽  
Author(s):  
Lan Xu ◽  
Liang Wang ◽  
Naeem Faraz

In this paper, a thermo-electro-hydrodynamic model of the vibration- electrospinning process is first established. The model can offer in-depth insight into physical understanding of many complex phenomena which can not be fully explained experimentally. It is a powerful tool to controlling over physical characters.


2014 ◽  
Vol 485-486 ◽  
pp. 828-841 ◽  
Author(s):  
Christian Siebert ◽  
Tino Rödiger ◽  
Ulf Mallast ◽  
Agnes Gräbe ◽  
Joseph Guttman ◽  
...  

1985 ◽  
Vol 16 (5) ◽  
pp. 273-290 ◽  
Author(s):  
J. Deschesnes ◽  
J.-P. Villeneuve ◽  
E. Ledoux ◽  
G. Girard

The MC model, developed to simulate the simultaneous movements of surface and groundwater flows in a watershed, is applied to three different types of watersheds to demonstrate its characteristics and its flexibility of use. The first case reports on an application where the surface flow and the groundwater flow are of the same importance, the second case reports on one where the surface runoff dominates and lastly we present a study where the groundwater flows are dominant. In each case, we place emphasis on how the MC model can integrate the hydrological system under study for an accurate representation of reality. Examples of results are also included.


2012 ◽  
Vol 8 (S291) ◽  
pp. 207-207
Author(s):  
Sarah Buchner

AbstractThe Vela pulsar, like many other young pulsars, undergoes occasional sudden “spin-ups” in rotational frequency known as glitches. These glitches are characterised by a sudden (less than 30s) rise in the rotation frequency accompanied by a jump in the spin-down. This is generally followed by rapidly decaying transients in the spin-down and a gradual linear recovery. This recovery provides insight into the internal structure of the neutron star.The telescopes at HartRAO was been used to monitor the Vela pulsar almost daily from 1985 in order to monitor these glitches. The vast majority of these observations were made using the 26m antenna at 1.6 GHz and 2.3 Ghz. When the 26m antenna was offline due to a bearing failure for two years from 2008 the 15m MeerKAT prototype antenna was used to observe Vela.During the entire monitoring campaign 10 large glitches have been observed. The majority of the glitches show a similar recovery pattern. We discuss the characteristics of this common recovery. We compare the standard glitch recovery to that predicted by a hydrodynamic model of the neutron star interior.An exception to the standard glitch are the two glitches which occurred in 1994 separated by 32 days. This “double” glitch is unique amongst Vela glitches. The event is accompanied by typical transients in rotation frequency derivative but all of the long-term offset occurs at the first event and the rapidly-decaying transient is only seen with the second spin-up.


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