Seismology Research at NMSU

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jive_in_nm [2024/07/12 22:33] – [Saturn] jasonjjive_in_nm [2024/08/02 19:09] (current) – [JIVE and Juno] jasonj
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 ===== Jovian Interiors Velocimetry Experiment in New Mexico ===== ===== Jovian Interiors Velocimetry Experiment in New Mexico =====
- The Jovian Interiors Velocimetry Experiment in New Mexico (JIVE in NM), a NASA-funded project, will determine the interior structure and composition of Jupiter using seismology. A sensitive imaging spectrometer will be built by close collaborators in Nice, France that can measure the confirmed oscillations of these planets to a precision high enough to enable detailed studies of the planetary interiors. Since the gas-giant planets played such a critical role in the formation of the Solar System, and since so little about their core and compositional properties is constrained by observation, the seismic discoveries we will make with JIVE will finally allow us to discriminate between competing theories of planetary formation. Furthermore, precise measurements of the atmospheric winds will uncover new details into the physical processes that drive the zonal jets, and provide the data necessary to carry out monitoring of Jovian climatology to understand its complex dynamics.+ The Jovian Interiors Velocimetry Experiment in New Mexico (JIVE in NM), a NASA-funded project, will determine the interior structure and composition of Jupiter using seismology. A sensitive imaging spectrometer has been designed and built with collaborators in Nice, France that can measure the confirmed oscillations of these planets to a precision high enough to enable detailed studies of the planetary interiors. Since the gas-giant planets played such a critical role in the formation of the Solar System, and since so little about their core and compositional properties is constrained by observation, the seismic discoveries we will make with JIVE will finally allow us to discriminate between competing theories of planetary formation. Furthermore, precise measurements of the atmospheric winds will uncover new details into the physical processes that drive the zonal jets, and provide the data necessary to carry out monitoring of Jovian climatology to understand its complex dynamics.
  
-JIVE in NM strongly aligns with several current and planned space missions carried out in the Planetary Division of NASA's Science Mission Directorate, such as Juno and Cassini. It will establish and foster important partnerships between New Mexico State University and the New Mexico Institute of Mining and Technology. It will strengthen ties to another major statewide facility, Los Alamos National Laboratory, through its interior modeling component. It expands the collaboration to scientists with critical expertise located at three NASA centers: Ames, the Jet Propulsion Laboratory, and Goddard Space Flight Center. Finally, it leverages the team's connections to a group of scientists and engineers in Nice, France who paved the way for this groundbreaking research by designing the initial instruments that demonstrated that Jupiter pulsates, and whose latest design we will adapt for JIVE.+JIVE in NM strongly aligns with several current and past space missions carried out in the Planetary Division of NASA's Science Mission Directorate, such as Juno and Cassini. It has established and fostered\ important partnerships between New Mexico State University and the New Mexico Institute of Mining and Technology. It expands the collaboration to scientists with critical expertise located at three NASA centers: Ames, the Jet Propulsion Laboratory, and Goddard Space Flight Center. Finally, it leverages the team's connections to a group of scientists and engineers in Nice, France who paved the way for this groundbreaking research by designing the initial instruments that demonstrated that Jupiter pulsates, and whose latest design we will adapt for JIVE.
  
 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.
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 NASA's critical planetary science goal is to answer the question "How did the Sun's family of planets originate and evolve?" Jupiter played a major role in the formation of our Solar System. However, the manner in which Jupiter formed is still debated. This is due to the fact that its interior composition and structure is so poorly known that it could contain as little as none or as much as 40 Earth masses of elements other than hydrogen and helium. A similar uncertainty exists for Saturn. For both planets, the mass of their cores - the seeds of planetary formation in the early Solar System - are only crudely constrained by current observations. The large uncertainties in our understanding of these two massive planets that motivate this project are portrayed in Fig. 1. NASA's critical planetary science goal is to answer the question "How did the Sun's family of planets originate and evolve?" Jupiter played a major role in the formation of our Solar System. However, the manner in which Jupiter formed is still debated. This is due to the fact that its interior composition and structure is so poorly known that it could contain as little as none or as much as 40 Earth masses of elements other than hydrogen and helium. A similar uncertainty exists for Saturn. For both planets, the mass of their cores - the seeds of planetary formation in the early Solar System - are only crudely constrained by current observations. The large uncertainties in our understanding of these two massive planets that motivate this project are portrayed in Fig. 1.
  
-The Jovian Interiors from Velocimetry Experiment in New Mexico (JIVE in NM) is a NASA EPSCoR project whose research activities are designed to address this question and determine for the first time the interior structure and composition of Jupiter and Saturn and to gain new insights into their dynamic atmospheres. This will be carried out by constructing an optimized instrument that is capable of detecting Jovian oscillations to allow for seismic measurements of the planetary interiors and direct inferences of atmospheric winds. It builds and improves upon the successful design of an instrument that provided the first ever confirmed oscillations on Jupiter. The seismic results obtained in this project will reduce the range in possible core mass and interior composition in Fig. 1 by a factor of 5-10, allowing us to finally discriminate between competing theories of planetary formation. +The Jovian Interiors from Velocimetry Experiment in New Mexico (JIVE in NM) is a NASA project (EPSCoR and Solar Systems Observations funding) whose research activities are designed to address this question and determine for the first time the interior structure and composition of Jupiter and Saturn and to gain new insights into their dynamic atmospheres. This will be carried using an optimized instrument that is capable of detecting Jovian oscillations to allow for seismic measurements of the planetary interiors and direct inferences of atmospheric winds. It builds and improves upon the successful design of an instrument that provided the first ever confirmed oscillations on Jupiter. The seismic results obtained in this project will reduce the range in possible core mass and interior composition in Fig. 1 by a factor of 5-10, allowing us to finally discriminate between competing theories of planetary formation. 
  
 ==== Jovian Seismology ==== ==== Jovian Seismology ====
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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: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) }}]+[{{: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)  }}] 
  
 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.
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 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 ====
 +
 +Here are some archives of past meetings. 
 +
 +  * [[http://astronomy.nmsu.edu/jasonj/JIVE/nasa_technical_review_2017.html|NASA Technical Monitor meeting]], June 26, 2017, Las Cruces, NM 
 +  * [[https://www-n.oca.eu/jovial2016/Kick-off_Avril2016/index.html|JOVIAL Kick-off meeting]], April 2016, Nice, France 
 +  * [[http://astronomy.nmsu.edu/jasonj/JIVE/pages/2014_12_team.html|Team kickoff meeting]], December 2014, Las Cruces, NM 
 +  * Meeting, October 2014, Nice, France 
jive_in_nm.1720823636.txt.gz · Last modified: 2024/07/12 22:33 by jasonj