Gonna Leave for A Short While...

[EminemBase]

Got diagnosis of Bipolar recently and have to adjust to meds and I only mention that because, I'm now 'on the sick' temporarily, to those not in the UK: I'm claiming benefits to help support me until I'm 'fit to work' which I never plan to be as I'll make my own money

But anyway, I have about three months before I have to basically get a job or show why I'm still not fit to work so I need to just zone in on my websites now and work like fuck. So I'm trying to cut out all unnecessary distractions (Facebook, MSN, Yahoo and all forums etc.) as it's just impossible for me to progress with them all going.

It's just too easy to avoid working.

And, not that anybody should give a flying fuck I mean, wow I'm not posting for a few months, big fucking news? - I know I know, but I'm an egotistical cocksucker and this is in the Backstage anyway so fuck you. 'You' there being any person that thinks that... and I just thought it, so fuck ME. Fuck me? no fuck YOU! (me).

Okay so. Back in a few months, peace - I never say that but on a forum largely comprised of US users and a lot of bedroom gangsters so... PEACE

[Satire]

Meh.

[EminemBase]

Meh.

Meh.

[Maybe]

Meh.

Meh.

Meh.


Isn't conformity great?

[Satire]

On the real though peace bro. Somehow the Bi-Polar thing doesn't surprise me. Hope things work out for you, I guess?

<3 Good Luck Base God

[Block]

some aspects of the formation and evolution of binaries containing white dwarfs, black holes and neutron stars are investigated.
In the first part the formation of observed single undermassive white dwarfs and double helium white dwarfs is studied. I conclude that the formation of single undermassive white dwarfs can be explained by the evolution of `binaries' consisting of a solar-like star and a massive planet or brown dwarf. A tidal instability causes the low-mass companion to be drawn into the solar-like star when it evolves up the giant branch, expelling the giants envelope, leaving a single undermassive white dwarf. I reconstructed the evolution of three observed double helium white dwarfs, using the unique core mass -- radius relation for giants with degenerate cores, to find the pre-mass-transfer orbital separations and came to the following conclusions: (i) The last mass-transfer phase can be described with the spiral-in formalism with high common-envelope efficiency. (ii) The first mass-transfer phase cannot be described by a spiral-in nor by stable mass transfer but can be described very well with a formalism based on the angular momentum balance, with one free parameter which for the three observed systems has a very similar value.

Further, I calculated the current population of close double white dwarfs and interacting white dwarfs (AM CVn stars) and concluded: (i) The recently proposed cooling curves for helium white dwarfs overestimate the luminosity for the lowest mass helium white dwarfs (ii) The fraction of double white dwarfs among all white dwarfs can only be brought into agreement with observations if the initial binary fraction is not above 50 % (iii) The model with an exponentially decaying star formation rate gives a slightly better fit to the observed period distribution for double white dwarfs than a constant star formation rate. For the AM CVn stars I conclude that in order to distinguish between different models and formation channels both the theory of helium accretion disks and the homogeneity and completeness of the observations (particularly regarding the distances to the AM CVn stars) need to be improved. I already started this by reducing and analyzing high-speed spectroscopic data of AM CVn itself and found, for the first time, a clear direct signature of the binary nature of AM CVn in its spectrum.

The study of black hole binaries led to two conclusions. The first is that the observed space velocities of black hole binaries imply that in the supernova in which the black hole was produced, some 30 -- 50\% of the mass of the exploding helium star was ejected from the system if the explosion was symmetric. The second is that the mass-loss rates for for Wolf-Rayet stars currently used in stellar evolution calculations still overestimate the mass loss, yielding very low masses for massive stars when they explode. A mass-loss law more in agreement with the observed values significantly increases these final masses, improving the possibility for the formation of black holes in binaries.

Finally I describe the population of binaries consisting of two compact objects, either white dwarfs, neutron stars or black holes and use these to calculate the unresolved noise background produced by double white dwarfs and calculate the population of resolved binaries and binaries with signals sufficiently strong that they may be detected above the noise level for the low-frequency gravitational wave detector in space (LISA).




You should have left before the pasta got cold. Now look what you've done.

[Maybe]

some aspects of the formation and evolution of binaries containing white dwarfs, black holes and neutron stars are investigated.
In the first part the formation of observed single undermassive white dwarfs and double helium white dwarfs is studied. I conclude that the formation of single undermassive white dwarfs can be explained by the evolution of `binaries' consisting of a solar-like star and a massive planet or brown dwarf. A tidal instability causes the low-mass companion to be drawn into the solar-like star when it evolves up the giant branch, expelling the giants envelope, leaving a single undermassive white dwarf. I reconstructed the evolution of three observed double helium white dwarfs, using the unique core mass -- radius relation for giants with degenerate cores, to find the pre-mass-transfer orbital separations and came to the following conclusions: (i) The last mass-transfer phase can be described with the spiral-in formalism with high common-envelope efficiency. (ii) The first mass-transfer phase cannot be described by a spiral-in nor by stable mass transfer but can be described very well with a formalism based on the angular momentum balance, with one free parameter which for the three observed systems has a very similar value.

Further, I calculated the current population of close double white dwarfs and interacting white dwarfs (AM CVn stars) and concluded: (i) The recently proposed cooling curves for helium white dwarfs overestimate the luminosity for the lowest mass helium white dwarfs (ii) The fraction of double white dwarfs among all white dwarfs can only be brought into agreement with observations if the initial binary fraction is not above 50 % (iii) The model with an exponentially decaying star formation rate gives a slightly better fit to the observed period distribution for double white dwarfs than a constant star formation rate. For the AM CVn stars I conclude that in order to distinguish between different models and formation channels both the theory of helium accretion disks and the homogeneity and completeness of the observations (particularly regarding the distances to the AM CVn stars) need to be improved. I already started this by reducing and analyzing high-speed spectroscopic data of AM CVn itself and found, for the first time, a clear direct signature of the binary nature of AM CVn in its spectrum.

The study of black hole binaries led to two conclusions. The first is that the observed space velocities of black hole binaries imply that in the supernova in which the black hole was produced, some 30 -- 50\% of the mass of the exploding helium star was ejected from the system if the explosion was symmetric. The second is that the mass-loss rates for for Wolf-Rayet stars currently used in stellar evolution calculations still overestimate the mass loss, yielding very low masses for massive stars when they explode. A mass-loss law more in agreement with the observed values significantly increases these final masses, improving the possibility for the formation of black holes in binaries.

Finally I describe the population of binaries consisting of two compact objects, either white dwarfs, neutron stars or black holes and use these to calculate the unresolved noise background produced by double white dwarfs and calculate the population of resolved binaries and binaries with signals sufficiently strong that they may be detected above the noise level for the low-frequency gravitational wave detector in space (LISA).




You should have left before the pasta got cold. Now look what you've done.

Hahahahahahahaha. When I read the first line, I spit out my snapple. Now it's all over the keyboard you bastard.

[VenomBlackViper]

Aw shit EminemBase is gone, someone better start taking some typing lessons real soon and fill in for him.

[Block]

Aw shit EminemBase is gone, someone better start taking some typing lessons real soon and fill in for him.

I could attempt to lower my grammatical standards and see what I can do.

[ThomasJ]

[Satire]

inb4

[Sam.]

c-ya a o
short and sweet

[Kevin Paul]

Find it funny that people are annoyed because embase writes to much.
Whats wrong with that? Would rather someone wrote a detailed post than some people who just comment "dope"

[DƎRDYPK]

inb4

peace EmBased

[VenomBlackViper]

inb4

peace EmBased

inafter