http://wikiet.gssi.it/index.php?action=history&feed=atom&title=Detector_configuration_and_scientific_potential 2026-05-23T12:01:04Z Revision history for this page on the wiki MediaWiki 1.32.0 http://wikiet.gssi.it/index.php?title=Detector_configuration_and_scientific_potential&diff=428&oldid=prev 2023-07-11T19:27:49Z

<p></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 19:27, 11 July 2023</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1" >Line 1:</td> <td colspan="2" class="diff-lineno">Line 1:</td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>[[File:Characteristic strains.png|Sensitivity models of LGWA and its pathfinder mission Soundcheck. The signal spectra <del class="diffchange diffchange-inline">show </del>an amplitude modulation caused by the rotation of the Moon. This modulation together with phase changes connected to the Moon's orbital motion around Earth and Sun allow precise sky-localization.|thumb|600px]]</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>[[File:Characteristic strains.png|Sensitivity models of LGWA and its pathfinder mission Soundcheck. The signal spectra <ins class="diffchange diffchange-inline">represent two months of observation time before merger. Most of the signals experience </ins>an amplitude modulation caused by the rotation of the Moon. This modulation together with phase changes connected to the Moon's orbital motion around Earth and Sun allow precise sky-localization.|thumb|600px]]</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The GW observation band of LGWA would span from about 1mHz to a few Hz. Over the lower part of the observation band, sensitivity will be limited by the noise of the seismometer used to read out the surface vibrations. At higher frequencies, it is possible that a seismic background forms a sensitivity limitation. The array configuration will allow us to disentangle lunar seismic events from GW signals, which effectively reduces the seismic background noise.  </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The GW observation band of LGWA would span from about 1mHz to a few Hz. Over the lower part of the observation band, sensitivity will be limited by the noise of the seismometer used to read out the surface vibrations. At higher frequencies, it is possible that a seismic background forms a sensitivity limitation. The array configuration will allow us to disentangle lunar seismic events from GW signals, which effectively reduces the seismic background noise.  </div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr> </table>

Jan.harms http://wikiet.gssi.it/index.php?title=Detector_configuration_and_scientific_potential&diff=427&oldid=prev 2023-07-11T19:26:47Z

<p></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 19:26, 11 July 2023</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1" >Line 1:</td> <td colspan="2" class="diff-lineno">Line 1:</td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>[[File:<del class="diffchange diffchange-inline">LGWA_CSIS</del>.png|LGWA <del class="diffchange diffchange-inline">sensitivity for two extreme lunar GW response models</del>.|thumb|600px]]</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>[[File:<ins class="diffchange diffchange-inline">Characteristic strains</ins>.png|<ins class="diffchange diffchange-inline">Sensitivity models of </ins>LGWA <ins class="diffchange diffchange-inline">and its pathfinder mission Soundcheck. The signal spectra show an amplitude modulation caused by the rotation of the Moon. This modulation together with phase changes connected to the Moon's orbital motion around Earth and Sun allow precise sky-localization</ins>.|thumb|600px]]</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The GW observation band of LGWA would span from about 1mHz to a few Hz. Over the lower part of the observation band, sensitivity will be limited by the noise of the seismometer used to read out the surface vibrations. At higher frequencies, it is possible that a seismic background forms a sensitivity limitation. The array configuration will allow us to disentangle lunar seismic events from GW signals, which effectively reduces the seismic background noise.  </div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The GW observation band of LGWA would span from about 1mHz to a few Hz. Over the lower part of the observation band, sensitivity will be limited by the noise of the seismometer used to read out the surface vibrations. At higher frequencies, it is possible that a seismic background forms a sensitivity limitation. The array configuration will allow us to disentangle lunar seismic events from GW signals, which effectively reduces the seismic background noise.  </div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr> </table>

Jan.harms http://wikiet.gssi.it/index.php?title=Detector_configuration_and_scientific_potential&diff=396&oldid=prev 2021-09-01T15:26:54Z

<p></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 15:26, 1 September 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l4" >Line 4:</td> <td colspan="2" class="diff-lineno">Line 4:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The question about the lunar GW response is not trivial to answer. An intuitive explanation of what happens requires the choice of a coordinate system. For example, in a local Lorentz frame, one must consider the change in coordinates of the seismometer proof mass with respect to the center of mass of the Moon. In this coordinate system, if the Moon did not respond to GWs at all, the seismometer would still see a GW signal since its proof mass would move with respect to an unresponsive lunar surface. Of course, there is a response of the Moon in a local Lorentz frame and it will amplify the GW signal seen by the seismometer at frequencies close to the normal-mode resonances, and it will dilute the GW signals off-resonance. How large the dilution is off-resonance has great influence on the overall GW response of the Moon, and it depends on geological details. Normal-mode simulations will provide more accurate models in the future.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The question about the lunar GW response is not trivial to answer. An intuitive explanation of what happens requires the choice of a coordinate system. For example, in a local Lorentz frame, one must consider the change in coordinates of the seismometer proof mass with respect to the center of mass of the Moon. In this coordinate system, if the Moon did not respond to GWs at all, the seismometer would still see a GW signal since its proof mass would move with respect to an unresponsive lunar surface. Of course, there is a response of the Moon in a local Lorentz frame and it will amplify the GW signal seen by the seismometer at frequencies close to the normal-mode resonances, and it will dilute the GW signals off-resonance. How large the dilution is off-resonance has great influence on the overall GW response of the Moon, and it depends on geological details. Normal-mode simulations will provide more accurate models in the future.</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Taking a more optimistic view on the LGWA sensitivity, it will be able to see a few binaries of neutron stars and solar-mass black holes together with mergers of massive black-hole binaries and many detections of white-dwarf binaries. Even though the detection of neutron star binaries would be rare, these would be observations of great importance since they would be used to issue alerts of an impending merger of these systems with precise sky location, which would allow the astronomers with EM facilities to prepare for these events.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Taking a more optimistic view on the LGWA sensitivity, it will be able to see a few binaries of neutron stars and solar-mass black holes together with mergers of massive black-hole binaries and many detections of white-dwarf binaries. Even though the detection of neutron star binaries would be rare, these would be observations of great importance since they would be used to issue alerts of an impending merger of these systems with precise sky location, which would allow <ins class="diffchange diffchange-inline">GW scientists and </ins>the astronomers with EM facilities to prepare for these events.</div></td></tr> </table>

Jan.harms http://wikiet.gssi.it/index.php?title=Detector_configuration_and_scientific_potential&diff=395&oldid=prev 2021-09-01T15:24:42Z

<p></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 15:24, 1 September 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l4" >Line 4:</td> <td colspan="2" class="diff-lineno">Line 4:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The question about the lunar GW response is not trivial to answer. An intuitive explanation of what happens requires the choice of a coordinate system. For example, in a local Lorentz frame, one must consider the change in coordinates of the seismometer proof mass with respect to the center of mass of the Moon. In this coordinate system, if the Moon did not respond to GWs at all, the seismometer would still see a GW signal since its proof mass would move with respect to an unresponsive lunar surface. Of course, there is a response of the Moon in a local Lorentz frame and it will amplify the GW signal seen by the seismometer at frequencies close to the normal-mode resonances, and it will dilute the GW signals off-resonance. How large the dilution is off-resonance has great influence on the overall GW response of the Moon, and it depends on geological details. Normal-mode simulations will provide more accurate models in the future.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The question about the lunar GW response is not trivial to answer. An intuitive explanation of what happens requires the choice of a coordinate system. For example, in a local Lorentz frame, one must consider the change in coordinates of the seismometer proof mass with respect to the center of mass of the Moon. In this coordinate system, if the Moon did not respond to GWs at all, the seismometer would still see a GW signal since its proof mass would move with respect to an unresponsive lunar surface. Of course, there is a response of the Moon in a local Lorentz frame and it will amplify the GW signal seen by the seismometer at frequencies close to the normal-mode resonances, and it will dilute the GW signals off-resonance. How large the dilution is off-resonance has great influence on the overall GW response of the Moon, and it depends on geological details. Normal-mode simulations will provide more accurate models in the future.</div></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr> <tr><td class='diff-marker'>−</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Taking a more optimistic view on the LGWA sensitivity, it will be able to see a few binaries of neutron stars and solar-mass black holes together with <del class="diffchange diffchange-inline">the </del>many detections of white-dwarf <del class="diffchange diffchange-inline">binaries and massive black-hole </del>binaries. Even though the detection of neutron star binaries would be rare, these would be observations of great importance since they would be used to issue alerts of an impending merger of these systems with precise sky location, which would allow the astronomers with EM facilities to prepare for these events.</div></td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Taking a more optimistic view on the LGWA sensitivity, it will be able to see a few binaries of neutron stars and solar-mass black holes together with <ins class="diffchange diffchange-inline">mergers of massive black-hole binaries and </ins>many detections of white-dwarf binaries. Even though the detection of neutron star binaries would be rare, these would be observations of great importance since they would be used to issue alerts of an impending merger of these systems with precise sky location, which would allow the astronomers with EM facilities to prepare for these events.</div></td></tr> </table>

Jan.harms http://wikiet.gssi.it/index.php?title=Detector_configuration_and_scientific_potential&diff=394&oldid=prev 2021-09-01T15:23:54Z

<p></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 15:23, 1 September 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l3" >Line 3:</td> <td colspan="2" class="diff-lineno">Line 3:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The question about the lunar GW response is not trivial to answer. An intuitive explanation of what happens requires the choice of a coordinate system. For example, in a local Lorentz frame, one must consider the change in coordinates of the seismometer proof mass with respect to the center of mass of the Moon. In this coordinate system, if the Moon did not respond to GWs at all, the seismometer would still see a GW signal since its proof mass would move with respect to an unresponsive lunar surface. Of course, there is a response of the Moon in a local Lorentz frame and it will amplify the GW signal seen by the seismometer at frequencies close to the normal-mode resonances, and it will dilute the GW signals off-resonance. How large the dilution is off-resonance has great influence on the overall GW response of the Moon, and it depends on geological details. Normal-mode simulations will provide more accurate models in the future.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The question about the lunar GW response is not trivial to answer. An intuitive explanation of what happens requires the choice of a coordinate system. For example, in a local Lorentz frame, one must consider the change in coordinates of the seismometer proof mass with respect to the center of mass of the Moon. In this coordinate system, if the Moon did not respond to GWs at all, the seismometer would still see a GW signal since its proof mass would move with respect to an unresponsive lunar surface. Of course, there is a response of the Moon in a local Lorentz frame and it will amplify the GW signal seen by the seismometer at frequencies close to the normal-mode resonances, and it will dilute the GW signals off-resonance. How large the dilution is off-resonance has great influence on the overall GW response of the Moon, and it depends on geological details. Normal-mode simulations will provide more accurate models in the future.</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Taking a more optimistic view on the LGWA sensitivity, it will be able to see a few binaries of neutron stars and solar-mass black holes together with the many detections of white-dwarf binaries and massive black-hole binaries. Even though the detection of neutron star binaries would be rare, these would be observations of great importance since they would be used to issue alerts of an impending merger of these systems with precise sky location, which would allow the astronomers with EM facilities to prepare for these events.</ins></div></td></tr> </table>

Jan.harms http://wikiet.gssi.it/index.php?title=Detector_configuration_and_scientific_potential&diff=393&oldid=prev 2021-09-01T15:19:05Z

<p></p> <table class="diff diff-contentalign-left" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #222; text-align: center;">Revision as of 15:19, 1 September 2021</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1" >Line 1:</td> <td colspan="2" class="diff-lineno">Line 1:</td></tr> <tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[File:LGWA_CSIS.png|LGWA sensitivity for two extreme lunar GW response models.|thumb|600px]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[File:LGWA_CSIS.png|LGWA sensitivity for two extreme lunar GW response models.|thumb|600px]]</div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">The GW observation band of LGWA would span from about 1mHz to a few Hz. Over the lower part of the observation band, sensitivity will be limited by the noise of the seismometer used to read out the surface vibrations. At higher frequencies, it is possible that a seismic background forms a sensitivity limitation. The array configuration will allow us to disentangle lunar seismic events from GW signals, which effectively reduces the seismic background noise. </ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr> <tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">The question about the lunar GW response is not trivial to answer. An intuitive explanation of what happens requires the choice of a coordinate system. For example, in a local Lorentz frame, one must consider the change in coordinates of the seismometer proof mass with respect to the center of mass of the Moon. In this coordinate system, if the Moon did not respond to GWs at all, the seismometer would still see a GW signal since its proof mass would move with respect to an unresponsive lunar surface. Of course, there is a response of the Moon in a local Lorentz frame and it will amplify the GW signal seen by the seismometer at frequencies close to the normal-mode resonances, and it will dilute the GW signals off-resonance. How large the dilution is off-resonance has great influence on the overall GW response of the Moon, and it depends on geological details. Normal-mode simulations will provide more accurate models in the future.</ins></div></td></tr> </table>

Jan.harms http://wikiet.gssi.it/index.php?title=Detector_configuration_and_scientific_potential&diff=392&oldid=prev 2021-09-01T14:58:26Z

<p>Created page with &quot;<a href="/index.php?title=File:LGWA_CSIS.png&amp;action=edit&amp;redlink=1" class="new" title="File:LGWA CSIS.png (page does not exist)">LGWA sensitivity for two extreme lunar GW response models.|thumb|600px</a>&quot;</p> <p><b>New page</b></p><div>[[File:LGWA_CSIS.png|LGWA sensitivity for two extreme lunar GW response models.|thumb|600px]]</div>

Jan.harms