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Revision of the properties of the GRS 1915+105 jets: Clues from the large-scale structure
Astrophysics · Submitted 11 May 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that by adapting a model for the radio lobes of extragalatic jet sources we predict a radio surface brightness of the equivalent structures of GRS 1915+105 below the current detection limits.
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The abstract, sentence by sentence
The jets of GRS 1915+105 carry a considerable energy away from the central source into the ISM. The similarity of the jets of this source and jets in radio galaxies or radio-loud quasars suggests that we should detect large-scale, synchrotron emitting radio structures surrounding GRS 1915+105. However, these large structures have not been found. We show that by adapting a model for the radio lobes of extragalatic jet sources we predict a radio surface brightness of the equivalent structures of GRS 1915+105 below the current detection limits. The model uses an energy transport rate of the jets averaged over the jet lifetime. This transport rate is found to be considerably lower than the power of the jets during the rare major ejection events. Thus the lobes contain less energy than would be inferred from these events and produce a lower radio luminosity. The model also predicts a lifetime of the jets of order $10^6$ years and a gas density of the ISM in the vicinity of GRS 1915+105 of $\sim 150$ cm$^{-3}$. The impact sites of the jets are identified with two {\sc iras} regions with a flat radio spectrum located on either side of GRS 1915+105. Observations of molecular lines and dust emission from these objects are consistent with our interpretation. Distance estimates for the {\sc iras} regions give 6.5 kpc and our model implies that this is also the distance to GRS 1915+105. This low distance estimate in combination with the observed motions of jet ejections on small scales yields a jet velocity of about 0.7 c and an angle of $53^{\circ}$ of the jets to our line of sight.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The jets of GRS 1915+105 carry a considerable energy away from the central source into the ISM. | background 0.99 | 0.14 | 0.06 | asserted 1.00 |
| s1 | The similarity of the jets of this source and jets in radio galaxies or radio-loud quasars suggests that we should detect large-scale, synchrotron emitting radio structures surrounding GRS 1915+105. | background 0.80 | 0.12 | 0.06 | hedged possibility 0.99 |
| s2 | However, these large structures have not been found. | gap 0.98 | 0.10 | 0.04 | asserted 1.00 |
| s3 | We show that by adapting a model for the radio lobes of extragalatic jet sources we predict a radio surface brightness of the equivalent structures of GRS 1915+105 below the current detection limits. | contribution 0.51 | 0.90 | 0.62 | asserted 1.00 |
| s4 | The model uses an energy transport rate of the jets averaged over the jet lifetime. | method 0.99 | 0.57 | 0.04 | asserted 0.99 |
| s5 | This transport rate is found to be considerably lower than the power of the jets during the rare major ejection events. | result 0.86 | 0.87 | 0.11 | asserted 1.00 |
| s6 | Thus the lobes contain less energy than would be inferred from these events and produce a lower radio luminosity. | interpretation 0.76 | 0.65 | 0.23 | asserted 1.00 |
| s7 | The model also predicts a lifetime of the jets of order $10^6$ years and a gas density of the ISM in the vicinity of GRS 1915+105 of $\sim 150$ cm$^{-3}$. | result 1.00 | 0.84 | 0.13 | asserted 0.89 |
| s8 | The impact sites of the jets are identified with two {\sc iras} regions with a flat radio spectrum located on either side of GRS 1915+105. | result 0.56 | 0.70 | 0.10 | asserted 0.99 |
| s9 | Observations of molecular lines and dust emission from these objects are consistent with our interpretation. | result 0.73 | 0.33 | 0.05 | hedged possibility 0.91 |
| s10 | Distance estimates for the {\sc iras} regions give 6.5 kpc and our model implies that this is also the distance to GRS 1915+105. | result 0.85 | 0.60 | 0.11 | asserted 0.97 |
| s11 | This low distance estimate in combination with the observed motions of jet ejections on small scales yields a jet velocity of about 0.7 c and an angle of $53^{\circ}$ of the jets to our line of sight. | result 0.92 | 0.82 | 0.16 | asserted 0.91 |
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Original abstract
The jets of GRS 1915+105 carry a considerable energy away from the central source into the ISM. The similarity of the jets of this source and jets in radio galaxies or radio-loud quasars suggests that we should detect large-scale, synchrotron emitting radio structures surrounding GRS 1915+105. However, these large structures have not been found. We show that by adapting a model for the radio lobes of extragalatic jet sources we predict a radio surface brightness of the equivalent structures of GRS 1915+105 below the current detection limits. The model uses an energy transport rate of the jets averaged over the jet lifetime. This transport rate is found to be considerably lower than the power of the jets during the rare major ejection events. Thus the lobes contain less energy than would be inferred from these events and produce a lower radio luminosity. The model also predicts a lifetime of the jets of order $10^6$ years and a gas density of the ISM in the vicinity of GRS 1915+105 of $\sim 150$ cm$^{-3}$. The impact sites of the jets are identified with two {\sc iras} regions with a flat radio spectrum located on either side of GRS 1915+105. Observations of molecular lines and dust emission from these objects are consistent with our interpretation. Distance estimates for the {\sc iras} regions give 6.5 kpc and our model implies that this is also the distance to GRS 1915+105. This low distance estimate in combination with the observed motions of jet ejections on small scales yields a jet velocity of about 0.7 c and an angle of $53^{\circ}$ of the jets to our line of sight.
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Therefore, radio maps would probably not be best suited for studying these interactions, as concluded by [ref] .
Interaction of a high-mass X-ray binary with the interstellar medium through stellar wind. The case of GX 301-2 · Discussion and conclusions · 0.99
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