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Detection of cosmic superstrings by geodesic test particle motion
High Energy Physics - Theory · Submitted 15 Dec 2010
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim While light deflection can also be caused by other matter distributions, the possibility of a negative perihelion shift seems to be a feature of finite width cosmic strings that could lead to the unmistakable identification of such objects.
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The abstract, sentence by sentence
(p,q)-strings are bound states of p F-strings and q D-strings and are predicted to form at the end of brane inflation. As such these cosmic superstrings should be detectable in the universe. In this paper we argue that they can be detected by the way that massive and massless test particles move in the space-time of these cosmic superstrings, in particular we study solutions to the geodesic equation in the space-time of field theoretical (p,q)-strings. The geodesics can be classified according to the test particle's energy, angular momentum and momentum in the direction of the string axis. We discuss how the change of the magnetic fluxes, the ratio between the symmetry breaking scale and the Planck mass, the Higgs to gauge boson mass ratios and the binding between the F- and D-strings, respectively, influence the motion of the test particles. While massless test particles can only move on escape orbits, a new feature as compared to the infinitely thin string limit is the existence of bound orbits for massive test particles. In particular, we observe that - in contrast to the space-time of a single Abelian-Higgs string - bound orbits for massive test particles in (p,q)-string space-times are possible if the Higgs boson mass is larger than the gauge boson mass. We also compute the effect of the binding between the p- and the q-string on observables such as the light deflection and the perihelion shift. While light deflection can also be caused by other matter distributions, the possibility of a negative perihelion shift seems to be a feature of finite width cosmic strings that could lead to the unmistakable identification of such objects. In Melvin space-times, which are asymptotically non-conical, massive test particles have to move on bound orbits, while massless test particles can only escape to infinity if their angular momentum vanishes.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | (p,q)-strings are bound states of p F-strings and q D-strings and are predicted to form at the end of brane inflation. | background 1.00 | 0.05 | 0.03 | asserted 0.88 |
| s1 | As such these cosmic superstrings should be detectable in the universe. | background 0.95 | 0.05 | 0.07 | hedged possibility 0.59 |
| s2 | In this paper we argue that they can be detected by the way that massive and massless test particles move in the space-time of these cosmic superstrings, in particular we study solutions to the geodesic equation in the space-time of field theoretical (p,q)-strings. | contribution 0.94 | 0.67 | 0.45 | hedged possibility 0.77 |
| s3 | The geodesics can be classified according to the test particle's energy, angular momentum and momentum in the direction of the string axis. | method 0.84 | 0.72 | 0.04 | asserted 1.00 |
| s4 | We discuss how the change of the magnetic fluxes, the ratio between the symmetry breaking scale and the Planck mass, the Higgs to gauge boson mass ratios and the binding between the F- and D-strings, respectively, influence the motion of the test particles. | contribution 0.85 | 0.70 | 0.05 | asserted 0.88 |
| s5 | While massless test particles can only move on escape orbits, a new feature as compared to the infinitely thin string limit is the existence of bound orbits for massive test particles. | result 1.00 | 0.82 | 0.23 | asserted 0.99 |
| s6 | In particular, we observe that - in contrast to the space-time of a single Abelian-Higgs string - bound orbits for massive test particles in (p,q)-string space-times are possible if the Higgs boson mass is larger than the gauge boson mass. | result 1.00 | 0.87 | 0.28 | asserted 0.86 |
| s7 | We also compute the effect of the binding between the p- and the q-string on observables such as the light deflection and the perihelion shift. | contribution 0.85 | 0.95 | 0.07 | asserted 1.00 |
| s8 | While light deflection can also be caused by other matter distributions, the possibility of a negative perihelion shift seems to be a feature of finite width cosmic strings that could lead to the unmistakable identification of such objects. | interpretation 0.73 | 0.71 | 0.23 | hedged possibility 0.97 |
| s9 | In Melvin space-times, which are asymptotically non-conical, massive test particles have to move on bound orbits, while massless test particles can only escape to infinity if their angular momentum vanishes. | result 0.90 | 0.45 | 0.07 | asserted 1.00 |
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The paper
Original abstract
(p,q)-strings are bound states of p F-strings and q D-strings and are predicted to form at the end of brane inflation. As such these cosmic superstrings should be detectable in the universe. In this paper we argue that they can be detected by the way that massive and massless test particles move in the space-time of these cosmic superstrings, in particular we study solutions to the geodesic equation in the space-time of field theoretical (p,q)-strings. The geodesics can be classified according to the test particle's energy, angular momentum and momentum in the direction of the string axis. We discuss how the change of the magnetic fluxes, the ratio between the symmetry breaking scale and the Planck mass, the Higgs to gauge boson mass ratios and the binding between the F- and D-strings, respectively, influence the motion of the test particles. While massless test particles can only move on escape orbits, a new feature as compared to the infinitely thin string limit is the existence of bound orbits for massive test particles. In particular, we observe that - in contrast to the space-time of a single Abelian-Higgs string - bound orbits for massive test particles in (p,q)-string space-times are possible if the Higgs boson mass is larger than the gauge boson mass. We also compute the effect of the binding between the p- and the q-string on observables such as the light deflection and the perihelion shift. While light deflection can also be caused by other matter distributions, the possibility of a negative perihelion shift seems to be a feature of finite width cosmic strings that could lead to the unmistakable identification of such objects. In Melvin space-times, which are asymptotically non-conical, massive test particles have to move on bound orbits, while massless test particles can only escape to infinity if their angular momentum vanishes.
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How the literature uses it
3 arXiv papers cite this in 4 sentences
Papers citing it · 1 sentence without a confident label
Cites it as background 3 papers
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Furthermore, the geodesic motion of test particles in field theoretical cosmic string spacetimes were investigated, namely Abelian-Higgs strings [ref] , two interacting Abelian-Higgs strings [ref] and cosmic superstrings [ref] .
Geodesic motion in the (rotating) black string spacetime · Introduction · 0.88
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Moreover, the motion of test particles was studied in various black string spacetimes [ref] including field theoretical cosmic string spacetimes [ref] and black holes pierced by a black string [ref] .
Analytic solutions of the geodesic equation for Einstein-Maxwell-dilaton-axion black holes · Introduction · 0.84
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Moreover, the solutions of the dynamical equations in the gravitational field of cosmic strings, such as Abelian-Higgs strings [ref] , two interacting Abelian-Higgs strings [ref] , and cosmic superstrings [ref] were mentioned in the paper [ref] .
Acceleration of particles in spacetimes of black string · Introduction · 0.98
What it cites · 2 sentences without a confident label
Compares with 2 papers
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In asymptotically flat black hole space-times and even asymptotically flat space-times of black holes pierced by infinitely thin cosmic strings (see [ref] ) the perihelion shift is positive.
The complete set of solutions of the geodesic equations in the space-time of a Schwarzschild black hole pierced by a cosmic string · Perihelion shift · 0.96
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In asymptotically flat black hole space-times and even asymptotically flat space-times of black holes pierced by infinitely thin cosmic strings (see [ref] ) the perihelion shift is positive.
Test particle motion in the space-time of a Kerr black hole pierced by a cosmic string · Perihelion shift · 0.96
Cites as background 4 papers
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The test particle motion in different space-times containing cosmic strings has been investigated in [ref] , while the complete set of orbits of test particles in the space-time of black hole pierced by an infinitely thin cosmic string has been given for a Schwarzschild black hole in [ref] and for a Kerr black hole in [ref] .
The complete set of solutions of the geodesic equations in the space-time of a Schwarzschild black hole pierced by a cosmic string · Introduction · 0.94
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The test particle motion in different space-times containing cosmic strings has been investigated in [ref] , while the complete set of orbits of test particles in the space-time of black hole pierced by an infinitely thin cosmic string has been given for a Schwarzschild black hole in [ref] and for a Kerr black hole in [ref] .
Test particle motion in the space-time of a Kerr black hole pierced by a cosmic string · Introduction · 0.94
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Though the identification of cosmic strings due to their gravitational lensing effects has been discussed extensively [ref] no such cosmic string lens has been detected to date.
The true nature of CSL-1 · Conclusions · 0.97
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