From: "Mike" <mike@acadex.ca>

Subject: IMPORTANT... Dr.A.B. McDonald...Neutrino Research

Date: Sat, 2 Jan 1999 04:50:08 -0500

Dear Dr. McDonald,

Please find attached, two interesting paragraphs of the studies made by

this group, that I have been following, along with the theory of

relativity. This along with my interest in your work with neutrinos has allowed me to make the statement that follows:

1. Let us label our space and time dimension as "Ground Zero" for easy

reference.

2. Let us label the dimensions exterior to this Ground Zero sphere as

Super-Atomic level 1,and that above SA-1 as SA-2 and SA-3 etc.etc.... to

infinity.

3. Let us label the dimensions interior to this Ground Zero sphere as

Atomic level 1, and that below A-1 as A-2 and A-3 etc.etc..... to

infinity.

4. We should assume that accurate physical equations at Ground Zero will

apply to any of these levels of dimensional spheres above and below

us,each higher level dimension is made up of the lower level . With

these assumptions we may also predict a dynamic constant that correlates

the accurate physical equations cross dimensionally. This constant will

involve the ratio of (GZ-time/GZ-molecular mass) AND

(SA-n-time/SA-n-mol.mass) for the Super-Atomic level OR

(A-n-time/A-n-mol.mass) for the Atomic level. (Where n is the

dimensional level in question.)

If my understanding of your neutrino experiment reasoning is accurate,

then there should be a reformation of neutrinos that may be viewed as a

loss, but in fact, that can be explained by the fact that the total

original mass must equal the total final mass. Where the total final

mass is equal to the total final mass in all dimensions. ENERGY IN ONE

DIMENSION IS MASS IN AN ANOTHER.

You can reach me at mike@acadex.ca and my day time phone number is

514-389-7297 ext.110, if you would like to discuss this subject.

Regards,

Mike Khouri

Montreal, Canada

20

20

Project: 3D Soliton Stars 20

J. Balakrishna, G. Daues, J. Mass F3, E. Seidel, W.-M. Suen, M. Tobias 20

Abstract 20

We have numerically evolved 1D Boson stars in the ground state and

the excited states, both with and without self-coupling. Spherically

symmetric perturbations have been used to test the stability of various

configurations. A lot of interesting physics has emerged from these

studies. Stable ground state boson stars with and without self-coupling

have very specific quasinormal modes of oscillations. These quasinormal

modes are a signature of stability and are very important in predicting

the final stable configuration that a perturbed boson star is going to

settle into. Excited states of boson stars are important because they

could be intermediate states during the formation process of boson

stars. These are inherently unstable. If they cannot lose enough mass

and make the transition to the ground state, they either form black

holes or, as in the case of configurations with M > N*m (where M 3D

mass of the star, N 3D number of bosons, m 3D mass of one boson) they

disperse to infinity. During the transition process of excited states to

ground states or black holes, these stars cascade through intermediate

states like atomic transitions. 20

The 3D problem, which we are now concentrating on, uses the G Code .

Not only is this an interesting physics problem, but it is also a

testbed of 3D spacetimes. We have made great strides in these 3D

evolutions. It also can be used as a source of gravitational waves. The

spherically symmetric problem (1D) involves scalar radiation. That is,

perturbed stars lose mass by scalar radiation. Nonspherical

perturbations result in gravitational waves. Evolving two

three-dimensional scalar field configurations and studying their

inspiral coalescence could have great astrophysical implications because

the gravitational waves emitted may not sensitively depend on the

internal structure of the compact objects. 20

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Project: General Relativistic Hydrodynamics 20

T. Font, M. Miller, W.-M. Suen, M. Tobias, and other members of the

NCSA/Potsdam/Wash U hydro team 20

Abstract 20

We have developed a fully general relativistic hydrodynamics

code (thorn_MAHC) based on high resolution shock capturing methods as a

general-purpose tool for research in relativistic astrophysics. The

hydrodynamic evolution is coupled to the spacetime evolution through the

cactus code. A version of the general relativistic hydro plus spacetime

code (GR3D) has recently been submitted to NASA with full documentation

as the second milestone code of the Neutron Star Coalescence Grand

Challenge Project. The code has been tested to run at over 140GFlops on

a 1024 node T3E. To obtain a copy of the code and see some of the

general relativistic hydro simulations carried out with it, please visit

GR3D Code . 20

Currently, the code has passed convergence tests on

Friedmann-Robertson-Walker cosmologies containing dust,

Oppenhiemer-Snyder dust collapse, shocktube problems,

Tolman-Oppenheimer-Volkoff (TOV) static stars, and boosted TOV stars. We

also have run neutron star head-on collisions and brill wave collisions

with neutron stars. Together with many other members of the

NCSA/Potsdam/Wash U hydro team, we are studying the long term stability

of general relativistic hydro simulations, the comparison of 3D

simulations with 1D and 2D simulations, and convergence tests of

rotating neutron stars. We will also be comparing 3D simulations to

perturbation studies. 20