This page contains the most important details of this project. If you find the information on this project inaccurate or inappropriate, please let us know by contacting us.
Submit Audition/Proposal on this Project
Rate this Project
Invitation Inbox
Project Main Details
Public Lead - 8737634 - Voice over needed for scientific animation
8737634
I need a documentary style reading for a scientific animation. I think it would be about 2 minutes long. It contains a lot of scientific vocabulary and should be read clearly and allow time for comprehension. I'm on a very small budget so please include your price.
Apr 24, 2006 15:46:58 (GMT -05:00) Eastern Time (US & Canada)
Apr 25, 2006 00:00:00 (GMT -05:00) Eastern Time (US & Canada)
No (click here to learn more about 
)
Closed
115
44
0 direct invitation(s) have been sent by the voice seeker resulting in 0 audition(s) and/or proposal(s) so far.
)
Closed
115
44
0 direct invitation(s) have been sent by the voice seeker resulting in 0 audition(s) and/or proposal(s) so far.
Project Parameters
None
To be defined
Promos
English - North American
Not defined
Young Adult Female OR Young Adult Male OR Middle Age Female OR Middle Age Male
Not defined
There are no special pre-, post-, or production requirements for this project.
Not defined
Not defined
No
Not defined
Script Details
Yes
FUL SCRIPT FOR PRICING REFERENCE//
How auroras are created:
The aurora borealis is a display of atmospheric glows that appears in the sky near the earth’s northern magnetic pole. It can also occur near the southern magnetic pole where it would be called the aurora australis. Although mostly green, auroras can also appear red and purple. Auroras occur in the earth’s ionosphere, starting at about 80 kilometers above ground and reaching up to 300 kilometers. Even at its lowest, an aurora reaches more than six times the height of a commercial jet’s flight.
But what causes these magnificent glows? The answer begins more than 90 million miles away in the corona of the sun. This is the outermost layer of the sun’s atmosphere and is on average about a million degrees centigrade. This extreme heat is enough to tear the electrons away from the hydrogen atoms in the atmosphere, creating a mix of very hot ions-- free electrons and positive protons. This is a state of matter known as plasma.
A hot temperature is just another way of saying that these ions have a high kinetic energy and that they are moving around very quickly. In fact, they travel so quickly that even the gravitational pull of the sun can’t keep them on the surface and they are ejected out into space. They flow out in every direction, creating a stream of plasma that is called the solar wind. About one million tons of these ions are blown off the sun every second. Even though they are traveling between 300 and 600 kilometers per second, the particles ejected from the sun still take three or four days to reach the earth.
Luckily, the earth has a strong magnetic field, called the magnetosphere, that protects us from this harmful radiation. The magnetosphere acts like a shield, deflecting most of the solar wind around the earth. The solar wind distorts the field, much like a comet is distorted, and creates a tail that flows away with the wind.
Where the solar wind first encounters the earth’s magnetic field there is a shock wave called the bow shock. Behind that are the weak magnetosheath and the distorted magnetosphere. On the night side of the planet is the magnetotail that extends awawy from the earth for more than 6 million kilometers, that’s the equivalent of 500 earth diameters.
While most of the protons and electrons of the solar wind are deflected away, many leak into the magnetosphere and become trapped in concentrated areas known as the Van Allen radiation belts. Here the ions travel up and down magnetic field lines, spiraling around them to maintain their kinetic energy. As the particles get near the magnetic poles, the concentration of field lines, or field strength, increases and acts to repel the ions. Here, the particle’s spiral motions are accelerated and its forward motion is slowed until, eventually, its direction is reversed and it travels along the field line to the opposite pole. For this reason, these locations are called mirror points.
At these mirror points, high energy electrons can drop out of the inner radiation belt and collide with atmospheric gases. The electron adds energy to the gas molecule and excites its electrons to a higher level. This higher level of energy is unstable so the molecule quickly returns to its natural state by releasing the stored energy as visible light— much the same way neon signs work. The wavelength or color of light varies for different gases. Oxygen at high altitudes produces a red aurora, while lower in the atmosphere it produces a yellow-green. Nitrogen can emit light that is blue or red-purple.
How auroras are created:
The aurora borealis is a display of atmospheric glows that appears in the sky near the earth’s northern magnetic pole. It can also occur near the southern magnetic pole where it would be called the aurora australis.
...................
.......................
How auroras are created:
The aurora borealis is a display of atmospheric glows that appears in the sky near the earth’s northern magnetic pole. It can also occur near the southern magnetic pole where it would be called the aurora australis. Although mostly green, auroras can also appear red and purple. Auroras occur in the earth’s ionosphere, starting at about 80 kilometers above ground and reaching up to 300 kilometers. Even at its lowest, an aurora reaches more than six times the height of a commercial jet’s flight.
But what causes these magnificent glows? The answer begins more than 90 million miles away in the corona of the sun. This is the outermost layer of the sun’s atmosphere and is on average about a million degrees centigrade. This extreme heat is enough to tear the electrons away from the hydrogen atoms in the atmosphere, creating a mix of very hot ions-- free electrons and positive protons. This is a state of matter known as plasma.
A hot temperature is just another way of saying that these ions have a high kinetic energy and that they are moving around very quickly. In fact, they travel so quickly that even the gravitational pull of the sun can’t keep them on the surface and they are ejected out into space. They flow out in every direction, creating a stream of plasma that is called the solar wind. About one million tons of these ions are blown off the sun every second. Even though they are traveling between 300 and 600 kilometers per second, the particles ejected from the sun still take three or four days to reach the earth.
Luckily, the earth has a strong magnetic field, called the magnetosphere, that protects us from this harmful radiation. The magnetosphere acts like a shield, deflecting most of the solar wind around the earth. The solar wind distorts the field, much like a comet is distorted, and creates a tail that flows away with the wind.
Where the solar wind first encounters the earth’s magnetic field there is a shock wave called the bow shock. Behind that are the weak magnetosheath and the distorted magnetosphere. On the night side of the planet is the magnetotail that extends awawy from the earth for more than 6 million kilometers, that’s the equivalent of 500 earth diameters.
While most of the protons and electrons of the solar wind are deflected away, many leak into the magnetosphere and become trapped in concentrated areas known as the Van Allen radiation belts. Here the ions travel up and down magnetic field lines, spiraling around them to maintain their kinetic energy. As the particles get near the magnetic poles, the concentration of field lines, or field strength, increases and acts to repel the ions. Here, the particle’s spiral motions are accelerated and its forward motion is slowed until, eventually, its direction is reversed and it travels along the field line to the opposite pole. For this reason, these locations are called mirror points.
At these mirror points, high energy electrons can drop out of the inner radiation belt and collide with atmospheric gases. The electron adds energy to the gas molecule and excites its electrons to a higher level. This higher level of energy is unstable so the molecule quickly returns to its natural state by releasing the stored energy as visible light— much the same way neon signs work. The wavelength or color of light varies for different gases. Oxygen at high altitudes produces a red aurora, while lower in the atmosphere it produces a yellow-green. Nitrogen can emit light that is blue or red-purple.
How auroras are created:
The aurora borealis is a display of atmospheric glows that appears in the sky near the earth’s northern magnetic pole. It can also occur near the southern magnetic pole where it would be called the aurora australis.
...................
.......................
Please note that you should only use the script or your recording of it for auditioning purposes. The script is property, unless otherwise specified, of the voice seeker and it is protected by international copyright laws.
Voice-Seeker Details
Voice123 Team Comments
Voice123 consultations with this voice seeker regarding this project and/or other projects by this voice seeker, via phone, chat, and/or email.
This project - phone.
Previous projects - phone.
This project - email or chat.
Previous projects - email or chat.
Corporate web site for this voice-seeker confirmed by Voice123
Note: Voice123 strives to establish the legitimacy of all projects posted. However, Voice123 subscribers and users are responsible for confirming information stated by prospective voice seekers, agents and/or clients. Voice123 subscribers and users assume all liability for use of any information found through Voice123, LLC, or any of its publications.
