- 데이터 포털
- 미국
- META URL
- https://catalog.data.gov/dataset/infrared-interferometry-of-auroral-ionosphere-thermosphere-energetics-project
- 라이선스
- notspecified
- 비용
- 제공기관
- National Aeronautics and Space Administration
- 관리부서
- 데이터
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The methodology developed under this grant is primarily an effort to develop new sub-payload technologies and an inexpensive method of testing them. The three technical goals are: (1) to improve and test the existing spring sub-payload ejection system and rocket propelled ejection system, (2) to test the performance of ampule-deployed radar chaff (rather than TMA) to track high altitude winds, and (3) to develop and test sensor and telemetry packages to monitor the attitude stability and position of deployed sub-payloads. The proposed effort will also demonstrate very low cost, low altitude rockets as an inexpensive flight test of payloads prior to expensive sounding rocket deployments. The payloads tested on 5 to 7 low-cost rockets will be (1) foil chaff designed for radar tracking of mesospheric winds, (2) plasma instruments composed of GPS monitors, magnetometers, and accelerometers, and (3) android phones for the investigation of off-the-shell instrumentation and telemetry. Finally, a campaign of 2 to 4 sounding rocket deployments on ‘as-available’ flights from Poker Flats will be used to test spring ejection without spin up, spring ejection with spin up for sub-payload attitude control, and rocket ejection
Methodology
Fly a high altitude sounding rocket with multiple sub-payloads to measure electric and magnetic fields during an auroral event. Use ground based observations to observe winds and conductivities in the ionosphere.
The Auroral Spatial Structures Probe (ASSP) is a NASA sounding rocket mission that, will be used to study both the spatial and temporal small scale variation of the E-fields during breakup aurora and geomagnetically active conditions. This will be accomplished through the use of a constellation of small payloads that separate relative to each other throughout a sounding rocket flight. The multiple baseline observations of the electric and magnetic fields will be used to observe variability of both the E-field and the Poynting flux. These observations will be placed in the context of available data, including winds, large scale E-fields, and proxy conductivity (airglow images) observations. In this way we will address the main scientific objective of this mission which is: What are the contributions of small spatial scale and rapid temporal scale fluctuations of electric fields relative to the larger-scale electrodynamic processes? The high altitude rocket will be launched along the magnetic field line and carry six sub-payloads to be ejected from the main payload at high velocity. The sub-payloads will be deployed both along the flight path and perpendicular to the flight path so that both spatial features and temporal-spatial ambiguities can be explored. The low-mass sub-payloads that, for a fixed ejection impulse will achieve at least a 50 km separation by the end of the flight are key to the observational success. Each sub-payload will carry a crossed pair of double-probe sensors to measure in-situ electric fields, a three axis magnetometer, a Langmuir probe and a GPS receiver. In this poster we review the ASSP science and mission concepts.
We propose a three-year effort to upgrade our existing sub-arcsecond Lyman-alpha telescope payload to improve the observing cadence by a factor of 2, increase the signal-to-ratio by a factor of 4, and launch the payload twice. With this upgraded performance, we will be able to investigate a number of scientific questions regarding the structure and heating of the solar atmosphere that address NASA’s Strategic Goal to understand the Sun and its effects on Earth and the Solar System. Specifically, the ultra-high resolution and high-temporal cadence VAULT2.0 science program and associated launch campaigns will answer the following five questions:
? What is the role of Type-II spicules in the transfer of energy and mass across the chromosphere-corona interface?
? Does neutral plasma absorption of the EUV emission from active region moss explain the discrepancies in the models of coronal loop heating?
? Where are the photospheric footpoints of coronal loops?
? What is the structure of coronal holes in the Lyman-alpha temperature range?
? What is the absolute abundance of H I at the base of the solar wind?
Despite decades of ground-based observations, the chromosphere remains one of the least understood layers of the solar atmosphere because of our limited understanding of the physical processes that govern it. In the last few years, the chromosphere has been propelled to the forefront of solar physics research thanks to spectacular new observations from space (Hinode/SOT and VAULT), and ground (e.g., SOUP, IBIS, DOT, SST), and the advent of sophisticated numerical simulations which are beginning to address the complex physics of the optically thick chromospheric plasmas and are opening up the interpretation of the observations. With these new capabilities come exciting new ideas regarding the role of the chromosphere in supplying the mass and energy to heat the corona, the nature of filaments, and the contribution of chromospheric jets to the solar wind. These ideas are challenging our traditional views of coronal heating (a long-standing mystery of solar physics), the existence of the ‘transition region’, the role of neutral plasmas in coronal emission and even the dominance of magnetic fields at coronal heights. The recent SMEX selection of a chromosphere-oriented mission, IRIS, is further evidence for the renewed importance of chromospheric physics. Observational limitations, however, are impeding further development and validation of these ideas. Both theoretical and observational considerations point to the importance of tracing the mass and energy on small spatial scales through the upper chromosphere and transition region (e.g., De Pontieu et al. 2007a, 2009, 2011; Vourlidas et al. 2010). This layer corresponds roughly to the temperature range from 10,000K (ground-based Hα) to 80,000K (space-based HeI). The requirement for high spatial- and temporal-resolution observations in this temperature range cannot be met fully by current instrumentation. Narrow-band, high-resolution images from TRACE, Hinode, STEREO and SOHO have inadequate temperature coverage or poor resolution. The SDO/AIA observations are skewed towards higher temperature plasmas. The SOHO spectrometers CDS and SUMER have good temperature coverage and fidelity, but limited spatial and temporal resolution and more importantly, limited operational lifetime. Hinode/EIS observations are mostly confined to the upper solar atmosphere while SOT observations are confined to the lower chromosphere (≤ 10,000K). The forthcoming IRIS satellite will partially cover the gap between chromosphere and transition region by obtaini