Seismology Research at NMSU

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jive_in_nm [2024/08/02 18:58] – [Jupiter's Atmosphere] jasonjjive_in_nm [2025/09/17 19:36] (current) – [Details of the Instrument] jasonj
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 This is a project of collaboration among undergraduate students, graduate students, faculty, and professional scientists and engineers geared towards ultimately solving fundamental questions in planetary science. This is a project of collaboration among undergraduate students, graduate students, faculty, and professional scientists and engineers geared towards ultimately solving fundamental questions in planetary science.
 +
 +==== Updates =====
 +__September 2025__. This is a unique year for Saturn as it's at equinox and its rings are mostly hidden from view. We received support from the New Mexico Space Grant Consortium to carry out observations at Saturn opposition. Fortunately, the sites in Japan and France are also operating and we hope to have some quasi-continuous data this year.
 +
 +Here is a tip-tilt animation of Saturn from September 16, 2025.
 +
 +{{ :wiki:jive:tiptilt_saturn.gif?nolink&300 |}}
 +
  
 ==== Motivation ==== ==== Motivation ====
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 By tracking the motion of visible clouds in the troposphere we know that the predominant weather pattern in the Jovian atmosphere consists of a series of alternating eastward and westward zonal jets that are remarkably steady over long time scales. We also know that, embedded between these alternating jets, other dynamical structures such as vortices and waves develop. Some of the most prominent of these features, like the Great Red Spot (GRS), are well characterized, and infrared observations indicate that Jupiter has a strong equatorial stratospheric jet.  By tracking the motion of visible clouds in the troposphere we know that the predominant weather pattern in the Jovian atmosphere consists of a series of alternating eastward and westward zonal jets that are remarkably steady over long time scales. We also know that, embedded between these alternating jets, other dynamical structures such as vortices and waves develop. Some of the most prominent of these features, like the Great Red Spot (GRS), are well characterized, and infrared observations indicate that Jupiter has a strong equatorial stratospheric jet. 
  
-[{{:wiki:science:vzonalmap.png?direct&200 |Fig. 3. Zonal velocity map from JIVE observations in 2019. The Great Red Spot is apparent. Similar maps of the meridional and vertical motions are also possible to estimate. JIVE will be able to distinguish wave motion and zonal flows, critical for understanding what powers the jets.  (Click for a larger image)  }}]+[{{:wiki:science:vzonalmap.png?direct&400 |Fig. 3. Zonal velocity map from JIVE observations in 2019. The Great Red Spot is apparent. Similar maps of the meridional and vertical motions are also possible to estimate. JIVE will be able to distinguish wave motion and zonal flows, critical for understanding what powers the jets.  (Click for a larger image)  }}]
  
-[{{:wiki:science:winds.png?direct&400 |Fig. 3. Example intensity image (top panel) whose clouds are tracked to give an estimated velocity map (bottom panel) within a zonal band on Jupiter. JIVE will be able to distinguish wave motion and zonal flows, critical for understanding what powers the jets.  (Click for a larger image) }}] 
  
 Despite the wealth of atmospheric information derived from ground-based observational campaigns and from space missions like Voyager and Galileo, many questions still remain unanswered. The mechanisms maintaing the dominant alternating jets, vortices and waves in the troposphere as well as their structure below the visible cloud level is largely unconstrained by the existing observations. The relationship between small-scale variability in the jets and the observed atmospheric morphology variability is also poorly understood. Finally, it remains unclear the precise role that eddies (large and small) and waves (large and small) play in governing Jupiter's weather pattern and its variability (both in the troposphere and in the stratosphere). Overall, the Jovian weather pattern is a complex system involving many different phenomena at different spatial and temporal scales, and we lack the continuous high-resolution observations of Jupiter's weather system as a whole needed to understand such dynamics. Despite the wealth of atmospheric information derived from ground-based observational campaigns and from space missions like Voyager and Galileo, many questions still remain unanswered. The mechanisms maintaing the dominant alternating jets, vortices and waves in the troposphere as well as their structure below the visible cloud level is largely unconstrained by the existing observations. The relationship between small-scale variability in the jets and the observed atmospheric morphology variability is also poorly understood. Finally, it remains unclear the precise role that eddies (large and small) and waves (large and small) play in governing Jupiter's weather pattern and its variability (both in the troposphere and in the stratosphere). Overall, the Jovian weather pattern is a complex system involving many different phenomena at different spatial and temporal scales, and we lack the continuous high-resolution observations of Jupiter's weather system as a whole needed to understand such dynamics.
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     * a frequency resolution of better than 1 muHz;     * a frequency resolution of better than 1 muHz;
     * accuracy of averaged zonal wind measurements in the Jovian atmosphere of approximately 1-2 m/s;      * accuracy of averaged zonal wind measurements in the Jovian atmosphere of approximately 1-2 m/s; 
 +
 +[{{ :wiki:science:jup_sat_dst.png?direct&300| Example images on the science CCD of Jupiter and Saturn taken with JIVE at the Dunn Solar Telescope in 2021.}}]
  
 No such Jovian ground-based instrument with these capabilities exists, nor does one for current or planned space missions to the giant planets. JIVE is an imaging spectrometer specifically designed to help achieve the scientific goals of this project and to meet these technical specifications. It will measure the Doppler shift in solar absorption lines from light that is reflected by clouds in Jupiter's upper troposphere, providing spatially resolved line-of-sight velocity images of the whole planet at that altitude. More precisely, JIVE is a Fourier transform tachometer that will simultaneously produce a visible image and a Doppler-velocity image of the planet at a regular temporal interval. No such Jovian ground-based instrument with these capabilities exists, nor does one for current or planned space missions to the giant planets. JIVE is an imaging spectrometer specifically designed to help achieve the scientific goals of this project and to meet these technical specifications. It will measure the Doppler shift in solar absorption lines from light that is reflected by clouds in Jupiter's upper troposphere, providing spatially resolved line-of-sight velocity images of the whole planet at that altitude. More precisely, JIVE is a Fourier transform tachometer that will simultaneously produce a visible image and a Doppler-velocity image of the planet at a regular temporal interval.
  
 +{{:wiki:jive:jupiter2.mp4?direct&350 | Europa and Jupiter. Credit: Sean Sellers}}
 Jovian oscillation periods and wavelengths dictate the rate and resolution that JIVE samples the surface velocity. Thus, JIVE is designed to provide Doppler-velocity images every 1 minute with a spatial resolution of about 1 arcsec (dependent on seeing), corresponding on average to about 3000 km on Jupiter (diameter of 140,000 km), or about 6000 km on Saturn (diameter of 120,000 km). The velocity images will be used to compute seismic observables like power spectra for mode identification, and can be averaged to obtain a latitudinal profile of winds sensitive to 1-2 m/s fluctuations. Jovian oscillation periods and wavelengths dictate the rate and resolution that JIVE samples the surface velocity. Thus, JIVE is designed to provide Doppler-velocity images every 1 minute with a spatial resolution of about 1 arcsec (dependent on seeing), corresponding on average to about 3000 km on Jupiter (diameter of 140,000 km), or about 6000 km on Saturn (diameter of 120,000 km). The velocity images will be used to compute seismic observables like power spectra for mode identification, and can be averaged to obtain a latitudinal profile of winds sensitive to 1-2 m/s fluctuations.
  
 JIVE is operated at the Dunn Solar Telescope at Sacramento Peak in Sunspot, NM.  JIVE is operated at the Dunn Solar Telescope at Sacramento Peak in Sunspot, NM. 
 +
 ==== JIVE and Juno ==== ==== JIVE and Juno ====
-[{{ :wiki:science:rt.png?direct&400|Fig. 4. JIVE and Juno are complementary. The blue box shows the interior range of Jupiter that will be possible to seismically explore with modes detected with JIVE. This includes a deep-interior program (light blue) using low-degree modes, and an envelope program (darker blue) for higher-degree up to l=25 when there is good telescope seeing. The red box shows the near-surface sensitivity possible from gravimetry with the Juno mission. Probe depths of a few example modes at the given frequencies and angular degree are shown (solid lines), as well as the expected transition locations for current Jupiter models (dashed lines). The x-scale is logarithmic. (Click for a larger image) }}]+[{{:wiki:science:rt.png?direct&400 |Fig. 4. JIVE and Juno are complementary. The blue box shows the interior range of Jupiter that will be possible to seismically explore with modes detected with JIVE. This includes a deep-interior program (light blue) using low-degree modes, and an envelope program (darker blue) for higher-degree up to l=25 when there is good telescope seeing. The red box shows the near-surface sensitivity possible from gravimetry with the Juno mission. Probe depths of a few example modes at the given frequencies and angular degree are shown (solid lines), as well as the expected transition locations for current Jupiter models (dashed lines). The x-scale is logarithmic. (Click for a larger image) }}]
  
 JIVE strongly aligns with NASA's Juno mission, whose primary scientific goal is to significantly improve our understanding of the formation, evolution and structure of Jupiter, and arrived at Jupiter in July 2016. Juno will make key contributions with precise measurements of Jupiter's gravity and magnetic fields and will radiometrically sound the deep atmosphere. While these gravitational measurements are primarily sensitive to the outer envelope of the planet, the acoustic waves that JIVE will measure propagate all the way to the core and are thus sensitive throughout the interior. Indeed, as Fig. 4 shows, JIVE is a perfect complement to Juno, and its observational campaigns will overlap with Juno's mission in Jupiter's orbit. Thus it extends Juno's capability, adds to its scientific return, and allows the possibility of critical cross-comparisons of results from two distinct types of measurements. JIVE strongly aligns with NASA's Juno mission, whose primary scientific goal is to significantly improve our understanding of the formation, evolution and structure of Jupiter, and arrived at Jupiter in July 2016. Juno will make key contributions with precise measurements of Jupiter's gravity and magnetic fields and will radiometrically sound the deep atmosphere. While these gravitational measurements are primarily sensitive to the outer envelope of the planet, the acoustic waves that JIVE will measure propagate all the way to the core and are thus sensitive throughout the interior. Indeed, as Fig. 4 shows, JIVE is a perfect complement to Juno, and its observational campaigns will overlap with Juno's mission in Jupiter's orbit. Thus it extends Juno's capability, adds to its scientific return, and allows the possibility of critical cross-comparisons of results from two distinct types of measurements.
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 Regarding seismology of Saturn, recent analysis by Hedman+ of occultation observations using the NASA Cassini spacecraft at Saturn shows exciting evidence of planetary modes that manifest themselves in its rings. This possibility was first proposed by team member Mark Marley and Carolyn Porco. The basic idea is that wave features in Saturn's C rings could be created by resonant interactions with internal oscillation modes, since these modes perturb the internal density profile and, therefore, the external gravity field. The observations of Hedman+ are the indirect evidence of these wave forcings. JIVE will be able to confirm this with direct observations of the global resonant oscillations on the planet. For a description of how the detailed features of these modes might be interpreted, see the excellent work by Jim Fuller.  Regarding seismology of Saturn, recent analysis by Hedman+ of occultation observations using the NASA Cassini spacecraft at Saturn shows exciting evidence of planetary modes that manifest themselves in its rings. This possibility was first proposed by team member Mark Marley and Carolyn Porco. The basic idea is that wave features in Saturn's C rings could be created by resonant interactions with internal oscillation modes, since these modes perturb the internal density profile and, therefore, the external gravity field. The observations of Hedman+ are the indirect evidence of these wave forcings. JIVE will be able to confirm this with direct observations of the global resonant oscillations on the planet. For a description of how the detailed features of these modes might be interpreted, see the excellent work by Jim Fuller. 
  
 +
 +==== Publications to date ====
 +
 +<bibtex furtherreading>
 +citetype=authordate
 +sort=false
 +
 +nocite=2024PSJ.....5..100S
 +nocite=2019Icar..319..795G
 +nocite=2017SPIE10401E..0YU
 +nocite=2012Icar..220..844J
 +
 +
 +</bibtex>
 ==== Meetings ==== ==== Meetings ====
  
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   * [[http://astronomy.nmsu.edu/jasonj/JIVE/pages/2014_12_team.html|Team kickoff meeting]], December 2014, Las Cruces, NM    * [[http://astronomy.nmsu.edu/jasonj/JIVE/pages/2014_12_team.html|Team kickoff meeting]], December 2014, Las Cruces, NM 
   * Meeting, October 2014, Nice, France    * Meeting, October 2014, Nice, France 
 +
 +==== Acknowledgements ====
 +
 +We'd like to express our deepest thanks for the following support for this project:
 +
 +  * New Mexico Space Grant Consortium Research Initiation Grant, "Seismic observations of ringless Saturn"  PI: Jackiewicz, CO-I: Markham, (2025-2026)
 +
 +  * NASA grant 80NSSC20K0672, Solar Systems Observations Program, "Near-continuous, ground-based, Doppler-velocity observations of solar-system gas giants to measure oscillations and atmospheric dynamics" PI: Jackiewicz, Co-I: Morales-Juberias, (2020-2025)
 +
 +  * NASA Cooperative Agreement #: NNX14AN67A, NASA EPSCoR, "Jovian Interiors from Velocimetry Experiment in New Mexico (JIVE in NM)" PI: Jackiewicz, (2014-2019)
 +
jive_in_nm.1722625089.txt.gz · Last modified: 2024/08/02 18:58 by jasonj