Diamond Nation Magazine & Summer IV 2010
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Vitilla: Now Sold at Diamond Nation
Beteyah, the first Trademark dedicated to the internationalization of the Vitilla Sport Game, can now be found in The Bullpen, Diamond Nation’s pro shop.
But what is Vitilla?
Originating in the Dominican Republic 30 years ago, Vitilla is the Dominican version of street baseball or stickball.
The Vitilla itself is a discarded plastic top of a gallon watercooler bottle.
You can play the game with or without bases.
If you are playing with bases, then you use regular baseball rules but without bases, outs are made differently.
If you catch the Vitilla while it’s in motion, then it’s considered an out. If the Vitilla comes to a complete a stop or you fumble it or don’t catch it, you are considered safe which equals a run.
You throw the Vitilla by grabbing it with your index finger and wrap it around the top layer and then your thumb wraps around the rest, so it looks like your hand is making an OK sign. You put your other fingers under the Vitilla and then you throw it.
If you throw with the Vitilla facing up, it leaves your hand like a fastball while if you throw it with the top down, the Vitilla turns into a curveball or dip.
While there are different motions, whether over the top or sidearm, the key is to get a steady grip and follow through.
What makes the game so great is you don’t need a lot of players and it’s portable.
All you need is a Vitilla and bat.
And if you are playing without a home plate and a catcher, then you can buy a circular wooden strike zone.
Last October was the 2nd Annual Red Bull Classico de Vitilla, one of the most popular sporting events in the Dominican Republic.
100 players grouped into 14 teams participated and after weeks of action, Los Bandoleros took first place.
Out of about 500 players from the Dominican Republic who have played in the Major Leagues, at least 80 percent have played Vitilla including superstars David Ortiz, Albert Pujols, Sammy Sosa and Pedro Martinez.
A number of Vitilla players have been scouted by Major League Baseball teams in the USA, and a lucrative contract in American baseball is the dream of every young Vitilla player in the Caribbean island country.
Nelson Geronimo, a neighborhood scout, the first contact for pro scouts and agents was quoted as saying, “The Vitilla is lateral, so it’s harder to hit.
It’s the best training for hand-eye coordination.
If you can hit a Vitilla, you can really hit a baseball.”
For more information, visit www.
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Proceedings of the twenty-second annual ACM-SIAM symposium on Discrete algorithms
San Francisco, California
& January 23 - 25, 2011
Society for Industrial and Applied Mathematics Philadelphia, PA, USA
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Save to BinderHydrodynamics of Cloud Collisions in Two Dimensions: The Fate of Clouds in a Mul
(arXiv:astro-ph/9706208)
Title:Hydrodynamics of Cloud Collisions in Two Dimensions: The Fate of Clouds in a Multiphase Medium
Authors:; ; ;
Affiliation:AA(School of Physics and Astronomy, 116 Church Street, SE, University of Minnesota, Minneapolis, MN 55455; , .; Dipartimento di Astronomia, Università di Firenze, I-50125 Firenze, Italy.), AB(School of Physics and Astronomy, 116 Church Street, SE, University of Minnesota, Minneapolis, MN 55455; , .), AC(Osservatorio Astrofisico Arcetri, Largo Enrico Fermi 5, I-50125 Firenze, I .), AD(Department of Astronomy and Space Science, Chungnam National University, Daejeon, 305-764, K .; Department of Astronomy, University of Washington, Box 351580, Seattle, WA .)
Publication:The Astrophysical Journal, Volume 491, Issue 1, pp. 216-232. ()
Publication Date:12/1997
Astronomy Keywords:Hydrodynamics, ISM: Clouds, ISM: Kinematics and Dynamics
Abstract Copyright:(c) 1997: The American Astronomical Society
Bibliographic Code:
We have studied head-on collisions between equal-mass, mildly supersonic
H I clouds (Mach number 1.5 with respect to the background medium)
through high-resolution numerical simulations in two dimensions. We
explore the role of various factors, including the radiative cooling
parameter, η = τrad/τcoll
(τcoll = Rc/vc), evolutionary
modifications on the cloud structure, and the symmetry of the problem.
Self-gravity is not included. Radiative losses are taken into account
explicitly and not approximated with an isothermal adiabatic index
γ ~ 1, which, in fact, leads to very different results. We assume
a standard two-phase interstellar medium (ISM) model where clouds are
characterized by a temperature Tc = 74 K and number density
nc = 22 cm-3 and are in pressure equilibrium with
the surrounding warm intercloud medium (WIM), with a density contrast
χ = ρc/ρi = 100. In particular, we
study collisions for the adiabatic (η && 1) and radiative
(η = 0.38) cases that may correspond to small (Rc &=
0.4 pc for an assumed WIM) or large (Rc ~ 1.5 pc) clouds,
respectively. In addition to a standard case of identical ``nonevolved''
clouds, we also consider the collision of identical clouds, ``evolved''
through independent motion within the intercloud gas, over one crushing
time before collision. This turns out to be about the mean collision
time for such clouds in the ISM. The presence of bow shocks and ram
pressure from material in the cloud wake alters these interactions
significantly with respect to the standard case. In some cases, we
removed the mirror symmetry from the problem by colliding initially
identical clouds ``evolved'' to different ages before impact. In those
cases, the colliding clouds have different density and velocity
structures, so that they provide a first insight on the behavior of more
complex interactions.
In our adiabatic collisions, the clouds are generally disrupted and
convert their gas into the warm phase of the ISM. Although the details
depend on the initial conditions, the two colliding clouds are converted
into a few low-density contrast (χ ~ 5) clumps at the end of the
simulations.
By contrast, for symmetric radiative cases, we find that the two clouds
coalesce, and there are good chances for a new massive cloud to be
formed. Almost all the initial kinetic energy of the two clouds is
radiated away during such collisions. On the other hand, for both
adiabatic and radiative collisions, symmetry breaking leads to major
differences. Most importantly, asymmetric collisions have a much greater
tendency to disrupt the two clouds. Portions of individual clouds may be
sheared away, and instabilities along the interfaces between the clouds
and with the intercloud medium are enhanced. In addition, radiative
cooling is less efficient in our asymmetric interactions, so that those
parts of the clouds that initially seem to merge are more likely to
reexpand and fade into the warm intercloud medium. Since the majority of
real cloud collisions should be asymmetric for one reason or another, we
conclude that most gasdynamical diffuse cloud collisions will be
disruptive, at least in the absence of significant self-gravity or a
significant magnetic field.
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