Line: 1 to 1  

VESF postdoctoral research fellowship at RMKI, Budapest  
Line: 15 to 14  
 
Changed:  
< <  to István Rácz <iracz@rmki.kfki.hu>.  
> >  to István Rácz .  
The letters of recommendations should be from faculty members or senior research scientists who are active in the field of study in question.
Applicants who submit their materials by February 15, 2009 will be given priority consideration. Review of applications will begin at that time and the position will be kept open until filled. Note that the position can exceptionally start before September 2009 if ask for.  
Changed:  
< <  Contact <iracz@rmki.kfki.hu> in case of any questions.  
> >  Contact in case of any questions.  
Changed:  
< <  For a detailed description, read this  
> >  A detailed description of the planned research program: here 
Line: 1 to 1  

 
Changed:  
< <  Open positions  
> >  VESF postdoctoral research fellowship at RMKI, Budapest  
Changed:  
< <  
> >  The Research Institute for Particle and Nuclear Physics (RMKI), Budapest invites applications from highly motivated candidates for a postdoctoral fellowship to be filled in the fall of 2009. The position is financed by the Virgo EGO Scientific Forum (VESF). The initial appointment is for one year renewable for up to two years. The appointment carries a salary, in accordance with the current official regulations for earlycareer research positions in Hungary, 16,000 EURO per annum with an additional allocation of up to 4,000 EURO for research support and 2,000 EURO for housing allowance. The selected candidate will have an opportunity to participate in the search for gravitational wave signals using the Virgo and LIGO detector data especially with planned joined science run expected to start from spring 2009.  
Deleted:  
< <  VESF Postdoctoral Fellowship (EGODIR1282008)  
Changed:  
< <  Production of readytouse gravitational wave templates for compact binary systems with the inclusion of spin and quadrupole effects and allowing eccentric and open orbits.  
> >  RMKI is an interdisciplinary research unit within the network of research institutes of the Hungarian Academy of Sciences. The Institute's activities include the following: field theory (in particular, theories of gravity), experimental and theoretical particle and nuclear physics, plasma physics, space science, and biophysics. The Virgo group of RMKI currently consists of four permanent researchers, two postdocs and two graduate students. The group has a good theoretical background in general relativity. Some of our ongoing projects are centered at the accurate description of the production and propagation of gravitational wave signals by making use of numerical relativity and the postNewtonian framework. The main task of the VESF postdoctoral fellow will be related to the application of these theoretical results in search for gravitational wave signals in the upcoming LIGOVirgo (S6 and VSR2) science run.  
Changed:  
< <  Background of research subject  
> >  To apply for the VESF postdoctoral research fellowship submit the following materials  
Changed:  
< <  The sensitivity of the new generation groundbased interferometric gravitational wave (GW) detectors has increased significantly. The associated developments certainly increase the chances of the first direct GW detection. While the first detection will be of great importance on its own right, presumably it will also teach us important lessons about gravitational interaction itself.  
> > 
 
Changed:  
< <  Currently the most widely accepted theory of gravity is general relativity, which is a metric theory of gravity. This implies, in particular, that the distribution and motion of matter fields and the spacetime metric are in an intimate relation. While the matter fields determine the spacetime geometry via Einstein's equations, the geometry is also involved in determining the evolution of matter fields via the pertinent field equations.  
> >  to István Rácz <iracz@rmki.kfki.hu>.  
Changed:  
< <  In general relativity the truly dynamical sources can only be treated by numerical and perturbative approaches. Whenever the gravitational field is weak and the motions are slow, the postNewtonian approximation is applicable for the description of the motion of the sources. To describe the emitted gravitational radiation far from the source, it has to be combined with the postMinkowskian multipolar expansion method. In this formalism, the evolution and the emitted waveform of black holes and/or neutron stars binaries can be described with sufficient precision.  
> >  The letters of recommendations should be from faculty members or senior research scientists who are active in the field of study in question.  
Changed:  
< <  The successful candidate will be expected to join to our ongoing research program aiming to determine the behaviour of astrophysically realistic binary systems and to provide readyto use gravitational waveform templates. This is done such that the various physical parameters, such as spins, quadrupole moments and the eccentricity of the orbits; and radiation reaction effects are taken into account.  
> >  Applicants who submit their materials by February 15, 2009 will be given priority consideration. Review of applications will begin at that time and the position will be kept open until filled. Note that the position can exceptionally start before September 2009 if ask for.  
Changed:  
< <  Research program and expected results:  
> >  Contact <iracz@rmki.kfki.hu> in case of any questions.  
Changed:  
< <  The most promising sources of gravitational radiation to be detected are compact binary systems composed of neutron stars and/or black holes in the last stage of their inspiral until the final plunge. To discuss the evolution of these systems to high precision the postNewtonian (PN) approximation is a convenient method when the gravitational field is weak and the motion of the sources are slow. For the detailed description of the emitted gravitational radiation the PN approximation is matched with the postMinkowskian multipolar expansion method in the near outer zone of the source system.
In the main stream investigations of the postNewtonian description of binary systems the principal aim was to achieve the highest possible PN; currently 3.5 PN order ; level since then the frequency of the associated GW signals is supposed to be high enough to be relevant for the groundbased interferometric GW detectors. This required the use of a great number of simplifying assumptions concerning the underlying binary system. For instance in most of the cases the investigations were restricted to the case of circular orbits and the spinorbit, spinspin and quadrupolemonopole interactions were completely neglected. During the last decade more and more investigations take into account these additional astrophysically important effects and the eccentricity of the orbits [1],[2]. There are important preliminary results concerning the full description of the motion of the binary [3], [4], nevertheless the equations of motion either are not solved or some of the above mentioned contributions are still missing. More than a decade ago an intensive study of the PN framework has been started under the leadership of Zoltán Perjés in our institute, at the KFKI Research Institute for Particle and Nuclear Physics. Our principal aim was to include all the astrophysically important effects in describing the motion of the binary and also to determine the created GW signals. Because these effects were missing from the former studies in our investigations we had to reproduce all the succeeding PN levels of corrections starting with the lowest order above the Newtonian. In the associated process we have given a new, detailed parametrization independent method in describing the motion of the binary system including the usual 1 PN corrections and spinorbit contributions manifest themselves through spin precession, orbital precession and orbital frequency ; and to determine the and polarization states of the emitted waveform [5],[6],[7] up to 1.5 PN order while keeping all the terms relevant for compact binaries. Our results contain the explicit description of the motion including angular evolution and the analytic form of the polarization states with the use of the generalized true anomaly parametrization [8]. Following the steps given in the general method we have given timedependent templates in the circular orbit limit. The associated results are currently written up for publication. These results justify the significance of the eccentricity of the orbits and the effects of the spinorbit interaction. For instance, the importance of spin effects on the waveform can be seen at 1.5 PN order in the equal or nearly equal mass case which is supposed to be highly relevant for neutron star binaries. Since the nonspinning contributions are all multiplied by the difference of the masses of the objects, the spinorbit interaction dominates the waveform at 1.5 PN order, in these particular cases. As opposed to this our first results demonstrate that in the general case the spin effects highly changes the characteristic properties of the waveforms even in the circular orbit special case from 1.5 PN order, although at lower orders these effects are definitely less significant. It is an important byproduct of the fact that the eccentricity of the orbits is also taken into account that higher harmonics of the waveforms appear in the analytic expressions. This effect enhances the probability of the detection of binary sources during the inspiralling era. The inclusion of the eccentricity is also supported by the fact that there has to be a significant fraction of the binaries, where the circularization of the orbits do not come to an end due to gravitational radiation in advance to the coalescence. Based on our present results the following three main research programs manifest themselves as the ones which can also be considered as natural continuation of our former investigations:
Bibliography:
Research environment such as group composition and experience, equipment:Our host institute, the KFKI Research Institute for Particle and Nuclear Physics of the Hungarian Academy of Sciences, shortly RMKI, is carrying out scientific research and related R&D activities in international collaborations. The main mission of RMKI is to conduct experimental and theoretical studies in particle and nuclear physics, gravitation and other field theoretical disciplines, plasma physics, space science and biophysics at an internationally recognized level. The main Hungarian centre for research in gravity, especially for general relativity, is also hosted by RMKI since the beginning of 70s. This theory group provided the core for the Hungarian VESF group, the MTAKFKIRMKI Group which joined to VESF in 2006 and which also involves researchers from the Eötvös University and from the University of Szeged. This year a new research group of RMKI has been formed which is dominated by experimental physicists aiming to participate in the VirgoEGO scientific collaboration. In the last meeting of the Virgo Scientific Committee the application of the RMKI group for the membership was approved. One of our main contributions for the Virgo EGO collaboration is to take part in the all sky search for GWs emitted by coalescing binaries formed by neutron stars and black holes with the inclusion of nonnegligible spin effects (Coalescing Binaries, CB, working group). With our present proposal we are aiming to open a VESF fellowship for theoretical research on GW detection. With the inclusion of a talented new postdoctoral fellow, whose main task will be to produce readytouse GW templates relevant for binary systems, we would like to strengthen the performance of the RMKI group. As for the guarantees ensuring the success of the VESF program is concerned, there are two members of the RMKIVirgo group, István Rácz and Mátyás Vasuth who are actively working in this field and are going to be able to provide scientific support for the newly applied postdoctoral fellow. In addition we would like to mention that the RMKI group is supported by advanced computing resources of our host institute. For instance, the largest cluster of HunGrid VO, the official Hungarian Virtual Organization of EGEE, is hosted by the computer centre of RMKI and administrated by the members of the RMKI group. This computational capacity will be suitable to produce the software injected fake GW signals and, if it will be needed, the new template banks for the Virgo scientific collaboration as it was indicated in details in the research plan.
The schedule and milestones of the research program:The research program is naturally structured by the principal aims addressed in the detailed research plan. An outline of this plan and the associated schedule can be given as follows: 1st year:
2nd year:
 
> >  For a detailed description, read this 
Line: 1 to 1  

Open positions  
Line: 6 to 6  
VESF Postdoctoral Fellowship (EGODIR1282008)  
Changed:  
< <  Readytouse gravitational wave templates for compact binary systems with the inclusion of spin and quadrupole effects and allowing eccentric and open orbits.  
> >  Production of readytouse gravitational wave templates for compact binary systems with the inclusion of spin and quadrupole effects and allowing eccentric and open orbits.  
Background of research subject  
Changed:  
< <  Due to the considerable international efforts, the sensitivity of the new generation of highly advanced groundbased interferometric gravitational wave (GW) detectors has increased significantly. In case of the LIGO and Virgo detectors, the associated developments increase the chances of the first direct GW detection, which will hopefully happen within the LSCVirgo collaboration in the near future. The first detection would be unique and important on its own right, but it would also teach us important lessons about gravitational interaction itself.  
> >  The sensitivity of the new generation groundbased interferometric gravitational wave (GW) detectors has increased significantly. The associated developments certainly increase the chances of the first direct GW detection. While the first detection will be of great importance on its own right, presumably it will also teach us important lessons about gravitational interaction itself.  
Currently the most widely accepted theory of gravity is general relativity, which is a metric theory of gravity. This implies, in particular, that the distribution and motion of matter fields and the spacetime metric are in an intimate relation. While the matter fields determine the spacetime geometry via Einstein's equations, the geometry is also involved in determining the evolution of matter fields via the pertinent field equations.  
Added:  
> >  
In general relativity the truly dynamical sources can only be treated by numerical and perturbative approaches. Whenever the gravitational field is weak and the motions are slow, the postNewtonian approximation is applicable for the description of the motion of the sources. To describe the emitted gravitational radiation far from the source, it has to be combined with the postMinkowskian multipolar expansion method. In this formalism, the evolution and the emitted waveform of black holes and/or neutron stars binaries can be described with sufficient precision.  
Added:  
> >  
The successful candidate will be expected to join to our ongoing research program aiming to determine the behaviour of astrophysically realistic binary systems and to provide readyto use gravitational waveform templates. This is done such that the various physical parameters, such as spins, quadrupole moments and the eccentricity of the orbits; and radiation reaction effects are taken into account.
Research program and expected results:  
Line: 18 to 21  
Research program and expected results:The most promising sources of gravitational radiation to be detected are compact binary systems composed of neutron stars and/or black holes in the last stage of their inspiral until the final plunge. To discuss the evolution of these systems to high precision the postNewtonian (PN) approximation is a convenient method when the gravitational field is weak and the motion of the sources are slow. For the detailed description of the emitted gravitational radiation the PN approximation is matched with the postMinkowskian multipolar expansion method in the near outer zone of the source system.  
Added:  
> >  
In the main stream investigations of the postNewtonian description of binary systems the principal aim was to achieve the highest possible PN; currently 3.5 PN order ; level since then the frequency of the associated GW signals is supposed to be high enough to be relevant for the groundbased interferometric GW detectors. This required the use of a great number of simplifying assumptions concerning the underlying binary system. For instance in most of the cases the investigations were restricted to the case of circular orbits and the spinorbit, spinspin and quadrupolemonopole interactions were completely neglected. During the last decade more and more investigations take into account these additional astrophysically important effects and the eccentricity of the orbits [1],[2]. There are important preliminary results concerning the full description of the motion of the binary [3], [4], nevertheless the equations of motion either are not solved or some of the above mentioned contributions are still missing.  
Added:  
> >  
More than a decade ago an intensive study of the PN framework has been started under the leadership of Zoltán Perjés in our institute, at the KFKI Research Institute for Particle and Nuclear Physics. Our principal aim was to include all the astrophysically important effects in describing the motion of the binary and also to determine the created GW signals. Because these effects were missing from the former studies in our investigations we had to reproduce all the succeeding PN levels of corrections starting with the lowest order above the Newtonian. In the associated process we have given a new, detailed parametrization independent method in describing the motion of the binary system including the usual 1 PN corrections and spinorbit contributions manifest themselves through spin precession, orbital precession and orbital frequency ; and to determine the and polarization states of the emitted waveform [5],[6],[7] up to 1.5 PN order while keeping all the terms relevant for compact binaries.  
Added:  
> >  
Our results contain the explicit description of the motion including angular evolution and the analytic form of the polarization states with the use of the generalized true anomaly parametrization [8]. Following the steps given in the general method we have given timedependent templates in the circular orbit limit. The associated results are currently written up for publication. These results justify the significance of the eccentricity of the orbits and the effects of the spinorbit interaction. For instance, the importance of spin effects on the waveform can be seen at 1.5 PN order in the equal or nearly equal mass case which is supposed to be highly relevant for neutron star binaries. Since the nonspinning contributions are all multiplied by the difference of the masses of the objects, the spinorbit interaction dominates the waveform at 1.5 PN order, in these particular cases. As opposed to this our first results demonstrate that in the general case the spin effects highly changes the characteristic properties of the waveforms even in the circular orbit special case from 1.5 PN order, although at lower orders these effects are definitely less significant. It is an important byproduct of the fact that the eccentricity of the orbits is also taken into account that higher harmonics of the waveforms appear in the analytic expressions. This effect enhances the probability of the detection of binary sources during the inspiralling era. The inclusion of the eccentricity is also supported by the fact that there has to be a significant fraction of the binaries, where the circularization of the orbits do not come to an end due to gravitational radiation in advance to the coalescence.  
Added:  
> >  
Based on our present results the following three main research programs manifest themselves as the ones which can also be considered as natural continuation of our former investigations:  
Changed:  
< <  1., The most straightforward is to complete our research at 1.5 PN order. This work includes the detailed investigation of the waveforms, the evaluation of readytouse GW templates, the determination of the effects of the different dynamical and geometrical parameters on the waveforms. An additional, more ambitious goal is to provide, based on our theoretical model, a method which can be applied in data analyzing processes to determine the astrophysical parameters (masses, spins, etc.) of the sources by making use of the detected GW signals. Our analytic results could also be useful in providing analytic initial conditions for numerical simulations describing coalescence. 2., The next reasonable step to do is the investigation of spinspin and quadrupolemonopole interactions at 2 PN order. The first one is mainly important in the case of BHBH and rapidly rotating BHNS, NSNS sources, and the second one is relevant in the case of slowly rotating NSNS binaries. Perhaps the importance of these effects is underlined by the fact that the inclusion of spinspin interaction is not compatible with the usual assumptions guaranteeing the circularization of the orbits [9].  
> > 
 
Along this line of investigations at first the spinprecession is to be discussed, and following this the decoupled angular equations can be given for the evolution of the system. With the help of these results the method for the evaluation of the polarization states will be worked out. The integration of the yielded equations requires a suitable generalization of the applied parametrization to include all the 2 PN corrections. Following this we will be able to integrate the equations of motion and provide a detailed description of the motion. With the use of the general method the explicit waveform contributions are also to be given. At this point the investigations of the 1.5 PN order results are to be repeated at the new level, and more accurate waveform templates will immediately be produced. In the next two years the possible endpoint of this line can be the investigation of the radiational reaction at 2.5 PN order. Since all the constants of the motion changes due to radiation, and since these constants play important role in our evaluation methods, technically it will be very challenging to incorporate this effect in our description. Nevertheless, it is important to be done, since it is crucial in describing the typical increase of the frequency of the; signal of the inspiralling binaries.  
Changed:  
< <  3., The investigation of binaries following parabolic or hyperbolic orbits is also very promising since they yield unique, nonperiodic and presumably strong enough GW signals. As former investigations show [10], the event rate is higher than one per year at the frequency range of the Virgo detector. Although these binaries appear to be relevant for the operating GW observatories, very few sufficiently detailed investigations of these types of systems have been done. The theoretical description of these sources is in a preliminary state, i.e., the parametrization of the orbit is available up to 1 PN order [11], and the description of the waveform is only at the Newtonian level.  
> > 
 
We plan to generalize our methods to investigate these sources. In doing so first we have to work out a suitable form of the parametrization of the orbit, and repeat the integration processes. Since the PN framework we have developed is already suitable to take into account various effects relevant for open orbits up to 1.5 PN order our results should extend without experiencing technical difficulties to the case of these systems. Finally, we would like to emphasize that once the detection of GW signals will become a daily practicethis is expected to happen once Advanced Virgo starts to operatethe most important goal will be to determine the physical properties of the sources of the observed GW signals. The above outlined research program promises that such a determination of the astrophysical parameters will be possible in case of the investigated sources. 
Line: 1 to 1  

Added:  
> > 
Open positions
VESF Postdoctoral Fellowship (EGODIR1282008)Readytouse gravitational wave templates for compact binary systems with the inclusion of spin and quadrupole effects and allowing eccentric and open orbits.
Background of research subjectDue to the considerable international efforts, the sensitivity of the new generation of highly advanced groundbased interferometric gravitational wave (GW) detectors has increased significantly. In case of the LIGO and Virgo detectors, the associated developments increase the chances of the first direct GW detection, which will hopefully happen within the LSCVirgo collaboration in the near future. The first detection would be unique and important on its own right, but it would also teach us important lessons about gravitational interaction itself. Currently the most widely accepted theory of gravity is general relativity, which is a metric theory of gravity. This implies, in particular, that the distribution and motion of matter fields and the spacetime metric are in an intimate relation. While the matter fields determine the spacetime geometry via Einstein's equations, the geometry is also involved in determining the evolution of matter fields via the pertinent field equations. In general relativity the truly dynamical sources can only be treated by numerical and perturbative approaches. Whenever the gravitational field is weak and the motions are slow, the postNewtonian approximation is applicable for the description of the motion of the sources. To describe the emitted gravitational radiation far from the source, it has to be combined with the postMinkowskian multipolar expansion method. In this formalism, the evolution and the emitted waveform of black holes and/or neutron stars binaries can be described with sufficient precision. The successful candidate will be expected to join to our ongoing research program aiming to determine the behaviour of astrophysically realistic binary systems and to provide readyto use gravitational waveform templates. This is done such that the various physical parameters, such as spins, quadrupole moments and the eccentricity of the orbits; and radiation reaction effects are taken into account.
Research program and expected results:The most promising sources of gravitational radiation to be detected are compact binary systems composed of neutron stars and/or black holes in the last stage of their inspiral until the final plunge. To discuss the evolution of these systems to high precision the postNewtonian (PN) approximation is a convenient method when the gravitational field is weak and the motion of the sources are slow. For the detailed description of the emitted gravitational radiation the PN approximation is matched with the postMinkowskian multipolar expansion method in the near outer zone of the source system. In the main stream investigations of the postNewtonian description of binary systems the principal aim was to achieve the highest possible PN; currently 3.5 PN order ; level since then the frequency of the associated GW signals is supposed to be high enough to be relevant for the groundbased interferometric GW detectors. This required the use of a great number of simplifying assumptions concerning the underlying binary system. For instance in most of the cases the investigations were restricted to the case of circular orbits and the spinorbit, spinspin and quadrupolemonopole interactions were completely neglected. During the last decade more and more investigations take into account these additional astrophysically important effects and the eccentricity of the orbits [1],[2]. There are important preliminary results concerning the full description of the motion of the binary [3], [4], nevertheless the equations of motion either are not solved or some of the above mentioned contributions are still missing. More than a decade ago an intensive study of the PN framework has been started under the leadership of Zoltán Perjés in our institute, at the KFKI Research Institute for Particle and Nuclear Physics. Our principal aim was to include all the astrophysically important effects in describing the motion of the binary and also to determine the created GW signals. Because these effects were missing from the former studies in our investigations we had to reproduce all the succeeding PN levels of corrections starting with the lowest order above the Newtonian. In the associated process we have given a new, detailed parametrization independent method in describing the motion of the binary system including the usual 1 PN corrections and spinorbit contributions manifest themselves through spin precession, orbital precession and orbital frequency ; and to determine the and polarization states of the emitted waveform [5],[6],[7] up to 1.5 PN order while keeping all the terms relevant for compact binaries. Our results contain the explicit description of the motion including angular evolution and the analytic form of the polarization states with the use of the generalized true anomaly parametrization [8]. Following the steps given in the general method we have given timedependent templates in the circular orbit limit. The associated results are currently written up for publication. These results justify the significance of the eccentricity of the orbits and the effects of the spinorbit interaction. For instance, the importance of spin effects on the waveform can be seen at 1.5 PN order in the equal or nearly equal mass case which is supposed to be highly relevant for neutron star binaries. Since the nonspinning contributions are all multiplied by the difference of the masses of the objects, the spinorbit interaction dominates the waveform at 1.5 PN order, in these particular cases. As opposed to this our first results demonstrate that in the general case the spin effects highly changes the characteristic properties of the waveforms even in the circular orbit special case from 1.5 PN order, although at lower orders these effects are definitely less significant. It is an important byproduct of the fact that the eccentricity of the orbits is also taken into account that higher harmonics of the waveforms appear in the analytic expressions. This effect enhances the probability of the detection of binary sources during the inspiralling era. The inclusion of the eccentricity is also supported by the fact that there has to be a significant fraction of the binaries, where the circularization of the orbits do not come to an end due to gravitational radiation in advance to the coalescence. Based on our present results the following three main research programs manifest themselves as the ones which can also be considered as natural continuation of our former investigations: 1., The most straightforward is to complete our research at 1.5 PN order. This work includes the detailed investigation of the waveforms, the evaluation of readytouse GW templates, the determination of the effects of the different dynamical and geometrical parameters on the waveforms. An additional, more ambitious goal is to provide, based on our theoretical model, a method which can be applied in data analyzing processes to determine the astrophysical parameters (masses, spins, etc.) of the sources by making use of the detected GW signals. Our analytic results could also be useful in providing analytic initial conditions for numerical simulations describing coalescence. 2., The next reasonable step to do is the investigation of spinspin and quadrupolemonopole interactions at 2 PN order. The first one is mainly important in the case of BHBH and rapidly rotating BHNS, NSNS sources, and the second one is relevant in the case of slowly rotating NSNS binaries. Perhaps the importance of these effects is underlined by the fact that the inclusion of spinspin interaction is not compatible with the usual assumptions guaranteeing the circularization of the orbits [9]. Along this line of investigations at first the spinprecession is to be discussed, and following this the decoupled angular equations can be given for the evolution of the system. With the help of these results the method for the evaluation of the polarization states will be worked out. The integration of the yielded equations requires a suitable generalization of the applied parametrization to include all the 2 PN corrections. Following this we will be able to integrate the equations of motion and provide a detailed description of the motion. With the use of the general method the explicit waveform contributions are also to be given. At this point the investigations of the 1.5 PN order results are to be repeated at the new level, and more accurate waveform templates will immediately be produced. In the next two years the possible endpoint of this line can be the investigation of the radiational reaction at 2.5 PN order. Since all the constants of the motion changes due to radiation, and since these constants play important role in our evaluation methods, technically it will be very challenging to incorporate this effect in our description. Nevertheless, it is important to be done, since it is crucial in describing the typical increase of the frequency of the; signal of the inspiralling binaries. 3., The investigation of binaries following parabolic or hyperbolic orbits is also very promising since they yield unique, nonperiodic and presumably strong enough GW signals. As former investigations show [10], the event rate is higher than one per year at the frequency range of the Virgo detector. Although these binaries appear to be relevant for the operating GW observatories, very few sufficiently detailed investigations of these types of systems have been done. The theoretical description of these sources is in a preliminary state, i.e., the parametrization of the orbit is available up to 1 PN order [11], and the description of the waveform is only at the Newtonian level. We plan to generalize our methods to investigate these sources. In doing so first we have to work out a suitable form of the parametrization of the orbit, and repeat the integration processes. Since the PN framework we have developed is already suitable to take into account various effects relevant for open orbits up to 1.5 PN order our results should extend without experiencing technical difficulties to the case of these systems. Finally, we would like to emphasize that once the detection of GW signals will become a daily practicethis is expected to happen once Advanced Virgo starts to operatethe most important goal will be to determine the physical properties of the sources of the observed GW signals. The above outlined research program promises that such a determination of the astrophysical parameters will be possible in case of the investigated sources. Bibliography:
Research environment such as group composition and experience, equipment:Our host institute, the KFKI Research Institute for Particle and Nuclear Physics of the Hungarian Academy of Sciences, shortly RMKI, is carrying out scientific research and related R&D activities in international collaborations. The main mission of RMKI is to conduct experimental and theoretical studies in particle and nuclear physics, gravitation and other field theoretical disciplines, plasma physics, space science and biophysics at an internationally recognized level. The main Hungarian centre for research in gravity, especially for general relativity, is also hosted by RMKI since the beginning of 70s. This theory group provided the core for the Hungarian VESF group, the MTAKFKIRMKI Group which joined to VESF in 2006 and which also involves researchers from the Eötvös University and from the University of Szeged. This year a new research group of RMKI has been formed which is dominated by experimental physicists aiming to participate in the VirgoEGO scientific collaboration. In the last meeting of the Virgo Scientific Committee the application of the RMKI group for the membership was approved. One of our main contributions for the Virgo EGO collaboration is to take part in the all sky search for GWs emitted by coalescing binaries formed by neutron stars and black holes with the inclusion of nonnegligible spin effects (Coalescing Binaries, CB, working group). With our present proposal we are aiming to open a VESF fellowship for theoretical research on GW detection. With the inclusion of a talented new postdoctoral fellow, whose main task will be to produce readytouse GW templates relevant for binary systems, we would like to strengthen the performance of the RMKI group. As for the guarantees ensuring the success of the VESF program is concerned, there are two members of the RMKIVirgo group, István Rácz and Mátyás Vasuth who are actively working in this field and are going to be able to provide scientific support for the newly applied postdoctoral fellow. In addition we would like to mention that the RMKI group is supported by advanced computing resources of our host institute. For instance, the largest cluster of HunGrid VO, the official Hungarian Virtual Organization of EGEE, is hosted by the computer centre of RMKI and administrated by the members of the RMKI group. This computational capacity will be suitable to produce the software injected fake GW signals and, if it will be needed, the new template banks for the Virgo scientific collaboration as it was indicated in details in the research plan.
The schedule and milestones of the research program:The research program is naturally structured by the principal aims addressed in the detailed research plan. An outline of this plan and the associated schedule can be given as follows: 1st year:
2nd year:
