00:00 We study the emissions and radiations continuously.
00:03 Now, we know that the Chandrayaan mission was successful at the time of 17 minutes of terror.
00:12 Now, it will take 125 days.
00:15 When will we know that the Aditya L1 mission was successful?
00:20 The first information will be available on Republic Day. It will take 110 days for the crew to reach L1.
00:30 After one week, all the shutters will be started.
00:36 By 26th January, Republic Day, we will get the results.
00:43 What are the challenges in the journey of Aditya L1?
00:47 There are four manoeuvres in the Earth-centric phases.
00:51 In the Earth-centric phases, we send the crew in the first orbit.
00:54 Then, the length of the orbit increases and Aditya L1 travels in the L1 direction to the fourth manoeuvre.
01:03 After reaching 1.5 million km, it will be in a particular orbit.
01:11 The orbital period of Aditya L1 is 177.86 days.
01:17 It will travel around the hollow orbit and continuously observe the Sun.
01:23 It will not be stable there. It will keep on rotating.
01:25 It can take. It will keep on rotating in the stable point.
01:29 Lagrangian point is a hollow orbit of lakhs of km.
01:36 It will take 177.86 days to reach the orbital period.
01:43 So, the satellites sent by NASA will travel in the same place?
01:50 The orbit will be different from Aditya L1.
01:53 There will be no disturbances.
01:56 Sir, Anil sir, we successfully sent the Mars Orbiter mission.
02:06 Will that experience be useful for Aditya L1?
02:09 Will the Earth's gravitational force be completely removed and the two will be in the same place?
02:20 Will the MAM experience be useful for us?
02:26 Yes, madam.
02:27 The point they chose is very important.
02:31 The reason they chose L1 is because the European Space Agency and ISRO have studied in detail.
02:39 Which point is a suitable point?
02:41 The reason they chose L1 is because the Earth's and the Sun's gravitational force is balanced.
02:49 In L1, the Earth's and the Sun's gravitational force are balanced.
03:03 So, the point is 1.5 km.
03:06 It is a suitable point for the Earth's and the Sun's gravitational force.
03:09 The Earth's and the Sun's gravitational force are balanced.
03:18 The data from the Earth's and the Sun's gravitational force is also helpful.
03:26 Many countries send satellites to the Earth's and the Sun's gravitational force.
03:32 Many satellites study the Earth's and the Sun's gravitational force.
03:37 They have gathered a lot of information.
03:40 The preliminary data from American scientists and other countries is very useful.
03:48 The preliminary data is available in the laboratory.
03:55 If we study the Earth's and the Sun's gravitational force in detail, we will get the complete information.
04:01 The data is useful for studying the solar winds, the elemental composition, the effects of solar winds on the Earth's and the Earth's gravitational force.
04:11 The data is useful for studying the solar winds, the elemental composition, the effects of solar winds on the Earth's and the Earth's gravitational force.
04:18 The data is useful for studying the solar winds, the elemental composition, the effects of solar winds on the Earth's and the Earth's gravitational force.
04:24 The satellite study is the main purpose of the satellite study.
04:29 Why couldn't the other countries do detailed study?
04:33 They did it years back.
04:39 We have a collaborative study.
04:45 We can choose the scientific development and discoveries at that time.
04:51 They are sending the data first.
04:54 We are not going for one study.
05:01 They have fixed one or two payloads for one study.
05:06 We will go for so many other studies.
05:11 We have added different payloads, spectrophotometers.
05:18 We will go for a complete study.
05:21 We are not going for a collaborative study.
05:26 We are going for a complete study.
05:31 We are going to study the chromosphere, photosphere, solar winds at L1 point, magnetic field, gravitational force.
05:41 We are going to do this study completely.
05:46 We are going to study this study with 7 payloads.
05:51 When the solar storm comes, the satellite study is disturbed.
05:59 How do you avoid the permanent damage of the satellite study?
06:11 Radio blackouts are more intense.
06:16 As it travels away from the sun, the energy slows down and the blackouts are diluted.
06:23 It is regained.
06:26 When the energy is more, the communication system is disturbed.
06:31 When it travels, the intensity and energy levels are reduced and it becomes normal.
06:37 The communication system is automatically regained.
06:41 Do you have to make all the satellites based on the conditions?
06:46 Yes.
06:47 In case of solar storms and all.
06:49 If the energy is more after the limit, it may damage the satellite.
06:58 After the damage, the satellite deviates from the orbit and collapses.
07:05 Has this ever happened?
07:07 Yes.
07:09 It has been recorded.
07:12 The power grid system in Canada was damaged.
07:15 If we explore the exact date, there is evidence.
07:22 In the remaining countries, SOHO is studying all the wavelengths.
07:26 There is SDO, Solar Dynamic Observatory.
07:29 They study the sun's position in every second.
07:35 In 2008, Parker Solar Probe was sent.
07:40 It is not near L1.
07:42 It is sent by the European Space Agency.
07:46 Is Parker closer to the sun?
07:49 It is near the sun, but not near L1.
07:51 It goes near the sun and takes images and returns.
07:56 Parker Solar Probe.
07:59 Solar Orbiter was sent in 2020 by the European Space Agency.
08:05 It concentrates on the solar wind.
08:09 Parker Solar Probe is also solar wind.
08:12 The temperature in the corona is a mystery.
08:17 In the photosphere, it is 6000 degrees Celsius.
08:20 It is low in the chromosphere.
08:22 It is maintained at 1 million degrees Celsius in the corona.
08:26 This is the mystery.
08:28 This is the primary goal.
08:30 We do different publications.
08:33 We analyze the solar wind and the temperature.
08:36 There are some reasons.
08:38 The corona heating process, magnetic reconnection process.
08:41 Magnetic reconnection is the solar flares time.
08:43 Magnetic reconnection is the magnetic field break and reconnect.
08:50 That is magnetic reconnection.
08:52 At that time, the solar energy particle speed varies.
08:56 When solar wind is used, solar eruptive phenomena occur.
09:01 On average, it comes at a speed of 400 km/s.
09:06 It comes at a speed of 400 km/s.
09:09 This is the average.
09:11 Maximum is 1500 km/s.
09:15 It comes with that speed.
09:17 If a huge solar flare occurs, it may exceed 1000 km/s.
09:24 It may exceed 1000 km/s to 1500 km/s.
09:28 That will definitely affect the magnetic field.
09:31 Geomagnetic storms may occur.
09:34 If geomagnetic storms occur,
09:37 if we consider the poles of the earth,
09:41 a spectacular phenomenon called aurora will occur.
09:46 Auroras occur when we go to high altitude regions,
09:50 to the poles of European countries.
09:53 When charged particles come at high speed
09:56 and touch the magnetic field of the earth,
10:01 the magnetic field of the earth is always in a closed loop.
10:06 It never breaks down.
10:09 The charged particles penetrate the magnetic field lines
10:16 and rotate to the poles of the earth.
10:23 The solar energy particles interact with the atmospheric constituents
10:28 like oxygen and nitrogen,
10:31 and a phenomenon called aurora is formed.
10:38 The auroras are different in color because
10:41 they are different atmospheric constituents.
10:44 The auroras are the result of solar eruptions.
10:52 These are all space weather prediction events.
10:55 Geomagnetic storms, auroras,
10:58 and ionosphere events are all predicted.
11:01 The ionosphere is affected by a sudden enhancement.
11:04 The flux of the ionosphere is enhanced.
11:07 If the ionosphere is suddenly enhanced,
11:10 we can predict the occurrence of an eruption.
11:15 The ionosphere is affected by a sudden enhancement.
11:18 The troposphere is affected by an increase in temperature.
11:22 The temperature increases in winter.
11:28 The temperature increases in winter.
11:33 You mentioned solar flares, solar winds, and solar storms.
11:38 What are the three major differences?
11:41 Geomagnetic storms are disturbances in the earth's magnetosphere.
11:48 Geomagnetic storms are caused by solar winds.
11:59 Geomagnetic storms are caused by solar winds.
12:05 Solar flares are caused by photosphere.
12:09 The brightness of the earth is suddenly enhanced due to magnetic reconnection.
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