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Overview
Overview
Have you ever seen the sun so close?
Can a body reach the sun?
Or it can reach it without getting burned.
Our dream came true when NASA launched a space probe called Parker, thanks to Dr. Eugene N. Parker, who helped develop the solar probe until it became The Parker Solar Probe, and now we know you're probably wondering a lot about this probe, so get ready Come with me and buckle up so we can start our journey with lots of information about this probe.
Definition of the parker probe
Definition of the parker probe
What is a probe? A space probe is a robotic spacecraft without a crew that does not orbit the Earth but is used to explore outer space as it is launched into outer space
Who is the regulator responsible for the Parker probe? Designed and built by the Johns Hopkins University Applied Physics Laboratory, and launched on August 12, 2018, the spacecraft cost 1.5 billion US dollars, and the probe's speed was calculated, which is 692,000 km / h
Do you think whether other purposes to launch this investigation?
Sure, it was also launched:
1) To know the secret related to the Corona region, which is at a distance of 3.5 to 13.2 million km from the surface of the sun and its temperature is about one million degrees Celsius... This is strange because the temperature on the surface of the sun is (6000 degrees) Celsius, so scientists believe that entering Parker's probe for this region may explain the reason for the high temperature in the Corona region.
2) Knowing the sources of the solar wind that comes out of the sun and spreads throughout the solar system.
3) Find out how solar wind particles travel through space at amazing speeds.
The probe will also be able to take samples of solar particles and magnetic fields so that scientists can find the answer to their questions about the stars around us.
Components of the parker probe
Components of the parker probe
First, let's start with Feilds (electromagnetic fields check).
The instrument kit captures the scale and shape of the electric and magnetic fields of the sun's atmosphere.
waves and perturbations in the inner heliosphere for a long time to understand regions associated with waves and shocks and to re-trace magnetic field lines.
Sensations measure the electric field around the spacecraft with five antennas.
Fields also measure electric fields over a wide bandwidth, either directly or at a distance. The four antennas work with sunlight, and they work in two modes to measure the characteristics of the fast and slow solar winds.
The fifth antenna protrudes perpendicular to the others in the shadow of the heat shield.
The suite contains three magnetometers to assess the magnetic field.
The first, the SCM, measures how the magnetic field is changing, and the other two, MAGi and Mago, measure the large-scale coronal magnetic field
let's go to the second instrument. ISIS.
let's go to the second instrument. ISIS.
The Integrated Science Investigation of the Sun — ISʘIS, pronounced “ee-sis” and including the symbol for the Sun in its acronym — uses two complementary instruments in one combined scientific investigation to measure particles across a wide range of energies. By measuring electrons, protons, and ions, ISʘIS will understand the particles’ lifecycles — where they came from, how they became accelerated and how they move out from the Sun through interplanetary space. The two energetic particle instruments on ISʘIS are called EPI-Lo and EPI-Hi (EPI stands for Energetic Particle Instrument).
EPI-Lo measures the spectra of electrons and ions and identifies carbon, oxygen, neon, magnesium, silicon, iron, and two isotopes of helium, He-3, and He-4. WhileEPI-Hi uses three particle sensors composed of stacked layers of detectors to measure particles with energies higher than those measured by EPI-Lo.
The third instrument is
WISPR (Wide-field Imager for Solar Probe) These optical telescopes acquire images of the corona and inner heliosphere. WISPR uses two cameras with radiation-hardened Active Pixel Sensor CMOS detectors. The camera's lenses are made of a radiation-hard BK7, a common type of glass used for space telescopes, which is also sufficiently hardened against the impacts of dust.
The last instrument is SWEAP (The Solar Wind Electrons Alphas and Protons Investigation).
It uses 2 main complementary instruments, SPAN and SPC. The instruments count the most abundant particles in the solar wind — electrons, protons, and helium ions — and measure such properties as velocity, density, and temperature to improve our understanding of solar wind and coronal plasma.
SPAN is composed of two instruments, SPAN-A and SPAN-B, which have wide fields of view to allow them to see the parts of space not observed by SPC.
SPC is what’s known as a Faraday cup, a metal device that can catch charged particles in a vacuum. Peeking over the heat shield to measure how electrons and ions are moving, the cup is exposed to the full light, heat, and energy of the sun.
There is a heat shield made of carbon and carbon foam, which consists of 97% air. It is a light-weight material that is easy to release into the air. This shield can withstand high heat waves of three million watts.
The square in the middle is the most efficient liquid cooling. It is made of titanium.
the track of the parker probe
The plot below shows the Parker Solar Probe's location and speed (relative to the Sun) as it conducts its science operations. The spacecraft is in a highly elliptical orbit around the Sun (the yellow dot at the center of the plot), reaching its aphelion during the course of the mission, initially at Earth and eventually close to the orbit of Venus. The Parker Solar Probe will perform seven Venus flybys in order to more precisely set its trajectory toward the Sun; these flybys will slow the spacecraft down instead of speeding it up, which is the more common use for planetary flybys.
Reading this chart:
Heliocentric velocity:
Speed in relation to the Sun; given in kilometers per second. One kilometer per second equals 0.62 miles per second or 2,237 miles per hour.
important theory
important theory
Scientists determined that the Sun had not a solid surface like Earth's but plasma.The reason that this plasma can be gathered and not made to fly into space is because of the gravitational and magnetic forces, the plasma is composed of charged ions, protons, and alpha particles that move from the Sun's surface into the Sun's atmosphere and return at very high speeds, but because of the increase in atmospheric temperature in excess of a million degrees. So fast and powerful are these particles that they overcome the force of the Sun's atmosphere, flying at high speeds in the solar system at 16,000,000 km/h, and if these rays could enter Earth, it was impossible to live on, because they carried deadly radiation, but what prevented these particles from entering Earth was the Earth's magnetic field, which is the planet's shield. This explains the aurorae that occur at Earth's poles, the appearance of color in the sky, caused by the solar wind colliding with the Earth's magnetic field
the achievements of the parker probe
In April, during the eighth round of the probe, The probe entered the Sun's atmosphere at 13 million km in the Corona region in December. The probe was able to take samples from inside. The Sun's atmosphere allows scientists to study the protons, ions, and alpha particles of the solar wind. It has been discovered that solar wind is caused by a crinkled structure on the surface of the Sun that contains giant columns of solar material called coronal signs, which borders the corona region. IT RISES INTO THE SUNS ATMOSPHERE AND IS CALLED THE GENERATING SURFACE. About a century ago, astronomer Henry Norris predicted the existence of a region free of cosmic dust around the Sun, which covers the entire solar system and presumably does not exist in the region around the Sun. By heating the dust particles with enough heat to make them disappear completely and cling to this zone (subduction zone). Scientists could not observe this area, but the Parker probe could observe it at a distance of 13.2 m km. It is said to begin 30.5 million km from the sun's surface.
However, the probe observed magnetic pathways from the photosphere, convincing them between structures called granules, which are giant bubbles on the surface of the Sun. The hot plasma rises from the Sun's interior, settles to the surface, and cools back into the Sun's interior. As plasma moves into and out of the Sun's interior, solar energy particles are the most energetic particles in the Sun that can overcome the Sun's gravity. Pushing out of the atmosphere in the form of solar winds. The probe was able to detect radio emissions from Venus' atmosphere and was able to photograph Venus for the first time with visible wavelengths.
Thus, the Parker probe has been able to bring many samples from the atmosphere that scientists can study and know much unknown information about the sun's atmosphere.
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