Information About The WISPR InstrumentThe WISPR instrument is made of two telescopes that are designed to sit between the two antennae from the fields experiment and image the solar wind and corona as were flying into it. So WISPR is the latest instrument. Scientists have built it for really two requirements, they wanted to able to see far from the spacecraft and then be able to track the structures that are flowing out from the sun, and then as they passed the spacecraft we would see them locally at the spacecraft.
The WISPR instrument is the only imaging instrument on the Parker Solar Probe and it is looking in the direction that these spacecraft are traveling and what it sees is lightly scattered by the dust that is in orbit about the sun. But then once we remove that what we see is the light scattered by the electrons in the corona, In the solar wind. These measurements that were made from the WISPR instrument have been made before by other instruments from 1 AU from the distance of the earth about one million miles from the sun.
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Parker Solar Probe cannot have any imager that looks at the sun directly. So the WISPR instrument looks off of the heat shield that protects us from this very intense. And so we sort of peak over the edge of it we use it as a shield to block out the sun itself and that allows us to see this very faint glow coming from the corona that is only observed during the clips. For example, we are creating an artificial Eclipse. What clip Cesare great but from the data point of view it looks instruments better. They are working continuously around the clock. Seven Days - A Week, 24 Hours - A Day, 365 Days - A Year.
Field ExperimentIn a special place on the spacecraft that the electronics package is inside the spacecraft. Where most of the Optronics is, but all of our sensors are mounted on the outside of the spacecraft. We have three sensors that measure magnetic fields that are mounted on a boom behind the spacecraft in the shadow shield and then we have five sensors that measure the plasma voltage. These are the electric field sensors. They extend into full sunlight and they get very hot.
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Two of the key measurements for understanding coronal heating are the measurement of the magnetic field and electric field. Together they give us what is called the Pointing Flux, which is the energy flux of the Corona. That measurement we have to actually go into that plasma and put sensors in the plasma to measure the magnetic field and electric field directly that is what fuels will do.
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There are two ways to measure electric fields in space. One is using a technique that is called a Double Problem then there is another technique which is measuring plasma waves or radio waves and fields. For the first time brings these two techniques together. I think the very first data we get will be revolutionary. At first blush, it will be a bunch of numbers as a function of time but the science team will take those numbers and make visualizations in the forms of spectrograms and eventually those data will be related to models and so we will be able to compare directly 3D visual models of the Coronal magnetic field.
These measurements have never been made in the environment close to the sun. We have made measurements similar to this in the earth's magnetosphere, iris ionosphere. But putting a package like this into the solar corona. It is just never done the closest anyone's ever been to the sun and based on what we have seen so far from spacecraft, not quite as close it is going to be striking.
ISOIS - Integrated Science Investigation Of The SunThe ISOIS investigation of the sun is an experiment that looks at energetic particles over a broad range of energies ( From tens of thousands of electron volts up to about a hundred million volts ). The ISOIS instrument is based on solid-state detectors. Those are detectors that when a particle passes through them, energy is deposited and you can measure that energy as well as you can measure that the particle is actually passed through. So there is the solar wind which is this continuous flow of lower energy particles and then there are much more sporadic and episodic events like solar flares that spew out the great number of these mean much more energetic particles.
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In our higher energy instrument, we have the whole set of layers of these detectors. When the particles pass through these layers it leaves energy in each and every one of those detectors. Those detectors are also segmented in pieces like a pie. So when a particle comes from a particular direction, you can tell both the direction, the particle came through and the energy and species of the particle by looking at all the different energy depositions.
In our lower energy instrument, we also have the same sort of solid-state detectors. But in addition to that, we use an extra trick. This is when a particle passes through a very thin foil it ejects an electron we are able to detect that and that gives us the start timing for the particle.
As we get closer and closer to the sun we will be able to differentiate between those two kinds of sources which will be more important to understanding the fundamentals of energetic particles in the solar system. By going in close and measuring the detailed distributions of these energetic particles, their energies, directions, and their species. We are going to learn that we could not possibly learn by looking from the remote distance. By understanding the sun in detail we can understand lots of other stars in much greater details
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