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Brissaud Q, Krishnamoorthy S, Jackson JM, Bowman DC, Komjathy A, Cutts JA, Zhan Z, Pauken MT, Izraelevitz JS, Walsh GJ. The First Detection of an Earthquake From a Balloon Using Its Acoustic Signature. GEOPHYSICAL RESEARCH LETTERS 2021; 48:e2021GL093013. [PMID: 34433991 PMCID: PMC8365762 DOI: 10.1029/2021gl093013] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/16/2021] [Revised: 04/20/2021] [Accepted: 04/23/2021] [Indexed: 06/13/2023]
Abstract
Extreme temperature and pressure conditions on the surface of Venus present formidable technological challenges against performing ground-based seismology. Efficient coupling between the Venusian atmosphere and the solid planet theoretically allows the study of seismically generated acoustic waves using balloons in the upper atmosphere, where conditions are far more clement. However, earthquake detection from a balloon has never been demonstrated. We present the first detection of an earthquake from a balloon-borne microbarometer near Ridgecrest, CA in July 2019 and include a detailed analysis of the dependence of seismic infrasound, as measured from a balloon on earthquake source parameters, topography, and crustal and atmospheric structure. Our comprehensive analysis of seismo-acoustic phenomenology demonstrates that seismic activity is detectable from a high-altitude platform on Earth, and that Rayleigh wave-induced infrasound can be used to constrain subsurface velocities, paving the way for the detection and characterization of such signals on Venus.
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Affiliation(s)
- Quentin Brissaud
- Seismological LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
- the Norwegian Seismic Array (NORSAR)OsloNorway
| | | | | | | | - Attila Komjathy
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - James A. Cutts
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Zhongwen Zhan
- Seismological LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Michael T. Pauken
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - Gerald J. Walsh
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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Krishnamoorthy S, Bowman DC, Komjathy A, Pauken MT, Cutts JA. Origin and mitigation of wind noise on balloon-borne infrasound microbarometers. THE JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA 2020; 148:2361. [PMID: 33138515 DOI: 10.1121/10.0002356] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/11/2020] [Accepted: 10/07/2020] [Indexed: 06/11/2023]
Abstract
High-altitude monitoring of low-frequency acoustic waves (infrasound) on Earth has regained prominence in recent years, primarily driven by improvements in light-weight sensor technology and advances in scientific ballooning techniques. Balloon-borne infrasound monitoring is also being proposed as a remote sensing technique for planetary exploration. Contrary to ground-based infrasound monitoring, the infrasound noise background in the stratosphere as measured by a balloon remains uncharacterized and the efficacy of wind noise mitigation filters has not been investigated. In this study, an analysis of pressure data collected using infrasound microbarometers during the flight of a long-duration zero pressure balloon is presented. A dramatic reduction of background noise in the stratosphere is demonstrated and it is shown that wind noise mitigation filters are not effective at reducing wind noise under these conditions. Results from this study demonstrate stratospheric balloons as a low-noise platform for infrasound monitoring and motivate the development of improved noise mitigation tools.
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Affiliation(s)
- Siddharth Krishnamoorthy
- National Aeronautics and Space Administration Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
| | - Daniel C Bowman
- Sandia National Laboratories, Albuquerque, New Mexico 87123, USA
| | - Attila Komjathy
- National Aeronautics and Space Administration Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
| | - Michael T Pauken
- National Aeronautics and Space Administration Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
| | - James A Cutts
- National Aeronautics and Space Administration Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
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Blamont JE, Young RE, Seiff A, Ragent B, Sagdeev R, Linkin VM, Kerzhanovich VV, Ingersoll AP, Crisp D, Elson LS, Preston RA, Golitsyn GS, Ivanov VN. Implications of the VEGA Balloon Results for Venus Atmospheric Dynamics. Science 2010; 231:1422-5. [PMID: 17748085 DOI: 10.1126/science.231.4744.1422] [Citation(s) in RCA: 48] [Impact Index Per Article: 3.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Both VEGA balloons encountered vertical winds with typical velocities of 1 to 2 meters per second. These values are consistent with those estimated from mixing length theory of thermal convection. However, small-scale temperature fluctuations for each balloon were sometimes larger than predicted. The approximate 6.5-kelvin difference in temperature consistently seen between VEGA-1 and VEGA-2 is probably due to synoptic or planetary-scale nonaxisymmetric disturbances that propagate westward with respect to the planet. There is also evidence from Doppler data for the existence of solar-fixed nonaxisymmetric motions that may be thermal tides. Surface topography may influence atmospheric motions experienced by the VEGA-2 balloon.
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Michael M, Tripathi SN, Borucki WJ, Whitten RC. Highly charged cloud particles in the atmosphere of Venus. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003258] [Citation(s) in RCA: 30] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Russell CT, Zhang TL, Wei HY. Whistler mode waves from lightning on Venus: Magnetic control of ionospheric access. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003137] [Citation(s) in RCA: 40] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Russell CT, Zhang TL, Delva M, Magnes W, Strangeway RJ, Wei HY. Lightning on Venus inferred from whistler-mode waves in the ionosphere. Nature 2007; 450:661-2. [DOI: 10.1038/nature05930] [Citation(s) in RCA: 85] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/23/2007] [Accepted: 05/01/2007] [Indexed: 11/09/2022]
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Gurnett DA, Zarka P, Manning R, Kurth WS, Hospodarsky GB, Averkamp TF, Kaiser ML, Farrell WM. Non-detection at Venus of high-frequency radio signals characteristic of terrestrial lightning. Nature 2001; 409:313-5. [PMID: 11201733 DOI: 10.1038/35053009] [Citation(s) in RCA: 70] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
The detection of impulsive low-frequency (10 to 80 kHz) radio signals, and separate very-low-frequency (approximately 100 Hz) radio 'whistler' signals provided the first evidence for lightning in the atmosphere of Venus. Later, a small number of impulsive high-frequency (100 kHz to 5.6 MHz) radio signals, possibly due to lightning, were also detected. The existence of lightning at Venus has, however, remained controversial. Here we report the results of a search for high-frequency (0.125 to 16 MHz) radio signals during two close fly-bys of Venus by the Cassini spacecraft. Such signals are characteristic of terrestrial lightning, and are commonly heard on AM (amplitude-modulated) radios during thunderstorms. Although the instrument easily detected signals from terrestrial lightning during a later fly-by of Earth (at a global flash rate estimated to be 70 s(-1), which is consistent with the rate expected for terrestrial lightning), no similar signals were detected from Venus. If lightning exists in the venusian atmosphere, it is either extremely rare, or very different from terrestrial lightning.
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Affiliation(s)
- D A Gurnett
- Department of Physics and Astronomy, The University of Iowa, Iowa City 52242, USA.
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Atkinson DH, Pollack JB, Seiff A. The Galileo Probe Doppler Wind Experiment: Measurement of the deep zonal winds on Jupiter. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/98je00060] [Citation(s) in RCA: 94] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Borucki WJ, Dyer JW, Phillips JR, Pham P. Pioneer Venus Orbiter search for Venusian lightning. ACTA ACUST UNITED AC 1991. [DOI: 10.1029/91ja01097] [Citation(s) in RCA: 45] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Russell CT, von Dornum M, Scarf FL. Planetographic clustering of low-altitude impulsive electric signals in the night ionosphere of Venus. Nature 1988. [DOI: 10.1038/331591a0] [Citation(s) in RCA: 21] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Abstract
In situ nightside electric field observations from the Pioneer Venus Orbiter have been interpreted as evidence of extensive lightning in the lower atmosphere of Venus. The scenario, including proposed evidence of clustering of lightning over surface highland regions, has encouraged the acceptance of currently active volcanic output as part of several investigations of the dynamics and chemistry of the atmosphere and the geology of the planet. However, the correlation between the 100-hertz electric field events attributed to lightning and nightside ionization troughs resulting from the interaction of the solar wind with the ionosphere indicates that the noise results from locally generated plasma instabilities and not from any behavior of the lower atmosphere. Furthermore, analysis of the spatial distribution of the noise shows that it is not clustered over highland topography, but rather occurs at random throughout the latitude and longitude regions sampled by the orbiter during the first 5 years of operation, from 1978 to 1984. Thus the electric field observations do not identify lightning and do not provide a basis for inferring the presence of currently active volcanic output. In the absence of known evidence to the contrary, it appears that Venus is no longer active.
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Linkin VM, Kerzhanovich VV, Lipatov AN, Shurupov AA, Seiff A, Ragent B, Young RE, Ingersoll AP, Crisp D, Elson LS, Preston RA, Blamont JE. Thermal Structure of the Venus Atmosphere in the Middle Cloud Layer. Science 1986; 231:1420-2. [PMID: 17748084 DOI: 10.1126/science.231.4744.1420] [Citation(s) in RCA: 32] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Thermal structure measurements obtained by the two VEGA balloons show the Venus middle cloud layer to be generally adiabatic. Temperatures measured by the two balloons at locations roughly symmetric about the equator differed by about 6.5 kelvins at a given pressure. The VEGA-2 temperatures were about 2.5 kelvins cooler and those of VEGA-1 about 4 kelvins warmer than temperatures measured by the Pioneer Venus Large Probe at these levels. Data taken by the VEGA-2 lander as it passed through the middle cloud agreed with those of the VEGA-2 balloon. Study of individual frames of the balloon data suggests the presence of multiple discrete air masses that are internally adiabatic but lie on slightly different adiabats. These adiabats, for a given balloon, can differ in temperature by as much as 1 kelvin at a given pressure.
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Linkin VM, Kerzhanovich VV, Lipatov AN, Pichkadze KM, Shurupov AA, Terterashvili AV, Ingersoli AP, Crisp D, Grossman AW, Young RE, Seiff A, Ragent B, Blamont JE, Elson LS, Preston RA. VEGA Balloon Dynamics and Vertical Winds in the Venus Middle Cloud Region. Science 1986; 231:1417-9. [PMID: 17748083 DOI: 10.1126/science.231.4744.1417] [Citation(s) in RCA: 43] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The VEGA balloons provided a long-term record of vertical wind fluctuations in a planetary atmosphere other than Earth's. The vertical winds were calculated from the observed displacement of the balloon relative to its equilibrium float altitude. The winds were intermittent; a large burst lasted several hours, and the peak velocity was 3 meters per second.
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Preston RA, Hildebrand CE, Purcell GH, Ellis J, Stelzried CT, Finley SG, Sagdeev RZ, Linkin VM, Kerzhanovich VV, Altunin VI, Kogan LR, Kostenko VI, Matveenko LI, Pogrebenko SV, Strukov IA, Akim EL, Alexandrov YN, Armand NA, Bakitko RN, Vyshlov AS, Bogomolov AF, Gorchankov YN, Selivanov AS, Ivanov NM, Tichonov VF, Blamont JE, Boloh L, Laurans G, Boischot A, Biraud F, Ortega-Molina A, Rosolen C, Petit G. Determination of Venus Winds by Ground-Based Radio Tracking of the VEGA Balloons. Science 1986; 231:1414-6. [PMID: 17748082 DOI: 10.1126/science.231.4744.1414] [Citation(s) in RCA: 53] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
A global array of 20 radio observatories was used to measure the three-dimensional position and velocity of the two meteorological balloons that were injected into the equatorial region of the Venus atmosphere near Venus midnight by the VEGA spacecraft on 11 and 15 June 1985. Initial analysis of only radial velocities indicates that each balloon was blown westward about 11,500 kilometers (8,000 kilometers on the night side) by zonal winds with a mean speed of about 70 meters per second. Excursions of the data from a model of constant zonal velocity were generally less than 3 meters per second; however, a much larger variation was evident near the end of the flight of the second balloon. Consistent systematic trends in the residuals for both balloons indicate the possibility of a solar-fixed atmospheric feature. Rapid variations in balloon velocity were often detected within a single transmission (330 seconds); however, they may represent not only atmospheric motions but also self-induced aerodynamic motions of the balloon.
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Kremnev RS, Linkin VM, Lipatov AN, Pichkadze KM, Shurupov AA, Terterashvili AV, Bakitko RV, Blamont JE, Malique C, Ragent B, Preston RA, Elson LS, Crisp D. VEGA Balloon System and Instrumentation. Science 1986; 231:1408-11. [PMID: 17748080 DOI: 10.1126/science.231.4744.1408] [Citation(s) in RCA: 37] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The VEGA Venus balloon radio transmissions received on Earth were used to measure the motion of the balloons and to obtain the data recorded by onboard sensors measuring atmospheric characteristics. Thus the balloons themselves, the gondolas, the onboard sensors, and the radio transmission system were all components of the experiment. A description of these elements is given, and a few details of data sampling and formatting are discussed.
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