TRANSFORMATION OF THE SOLAR SYSTEM
We will list the recent large-scale events in the Solar System in
order to fully understand, and comprehend, the Planeto - Physical
transformations taking place. This development of events, as it has
become clear in the last few years, is being caused by material and
energetic non-uniformity's in space. In its travel through interstellar
space, the Heliosphere on its way met non-homogeneities of matter and
energy This kind of interstellar space dispersed plasma is
presented by magnetized strip structures. The Heliosphere [solar
system] transition through this structure has led to an increase of the
shock wave in front of the Solar System from 3 to 4 AU, to 40 AU, or
more. This shock wave thickening has caused the formation of a
collusive plasma in a parietal layer, which has led to a plasma
overdraft around the Solar System, and then to its breakthrough into
interplanetary domains. This breakthrough constitutes a kind of energy
donation made by interplanetary space to our Solar System. In response
to this donation of energy/matter," we have observed a number of large
scale events:
A series of large Planeto-Physical transformations. A change in the
quality of interplanetary space in the direction of an increase in its
interplanetary, and solar-planetary transmitting properties.
The appearance of new states, and activity regimes, of the Sun.
The following processes are taking place on the distant planets of our
Solar System. But they are, essentially speaking, operationally driving
the whole System. Here are examples of these events:
A growth of dark spots on Pluto.
Reporting of auroras on Saturn.
Reporting of Uranus and Neptune polar shifts (They are magnetically
conjugate planets), and the abrupt large-scale growth of Uranus
magnetosphere intensity.
A change in light intensity and light spot dynamics on Neptune.
The doubling of the magnetic field intensity on Jupiter, and a series
of new states and processes observed on this planet as an aftermath of
a series of explosions in July 1994! That is, a relaxation of a
plasmoid train which excited the Jovian magnetosphere, thus
inducing excessive plasma generation and it's release
in the same manner as Solar coronal holes inducing an appearance of
radiation belt brightening, and the appearance of large auroral
anomalies and a change of the Jupiter - Io system of currents!
Update Note From Alex Dmitriev, Nov. 1997. A stream of ionized
hydrogen, oxygen, nitrogen, etc. is being directed to Jupiter from the
volcanic
areas of Io (the Moon of Jupiter) through a one million amperes flux
tube. It
is affecting the character of Jupiter's magnetic process and
intensifying it's Plasma.
Z.I.Vselennaya "Earth and Universe" N3, 1997 , 9 by NASA. A series of
Martian atmosphere transformations increasing its biosphere quality. In
particularly, a cloudy growth in
the equator area and an unusual growth of ozone concentration.
In September 1997 the Mars Surveyor Satellite encountered an
atmospheric density double that projected by NASA upon entering a Mars
orbit. This greater density bent one of the solar array arms beyond the
full and open stop. This combination of events has delayed the
beginning of the scheduled photo mission for one year. A first stage
atmosphere generation on the Moon, where a growing natrium atmosphere
is detected that reaches 9,000 km in height. Significant physical,
chemical and optical changes observed on Venus; an inversion of dark
and light spots detected for the first time, and a sharp decrease of
sulfur-containing gases in its atmosphere. A Change in the Quality of
Interplanetary Space Towards an Increase in Its Interplanetary and
Solar-Planetary Transmitting Properties. When speaking of new energetic
and material qualities of interplanetary space, we must first point out
the increase of the interplanetary domains energetic charge, and level
of material saturation. This change of the typical mean state of
interplanetary space has two main causes:
The supply/inflow of matter from interstellar space. (Radiation
material, ionized elements, and combinations.)
The after effects of Solar Cycle 22 activity, especially as a result of
fast coronal mass ejection's [CME's] of magnetized
solar plasmas.
It is natural for both interstellar matter and intra-heliospheric mass
redistribution's to create new structural units and processes in the
interplanetary domains. They are mostly observed in the structured
formation of extended systems of magnetic
plasma clouds, and an increased frequency of the generation of shock
waves; and their resulting effects.
A report already exists of two new populations of cosmic particles that
were not expected to be found in the Van Allen radiation belts;
particularly an injection of a greate, dense electron sheaf into the
inner magnetosphere during times of abrupt magnetic storms [CME's], and
the emergence of a new belt consisting of ionic elements traditionally
found in the composition of stars. This newly changed quality of
interplanetary space not only performs the function of a planetary
interaction transmission mechanism, but it (this is most important)
exerts stimulating and programming action upon the Solar activity both
in it's maximal and minimal phases.
The Appearance of New States and
Activity Regimes of the Sun.
As far as the stellarphysical state of the Sun is concerned, we
must first note the fact that significant modifications have occurred
in the existing behavioral model of the central object of our solar
system. This conclusion comes from observations and reportings of
unusual forms, energetic powers, and activities in the Sun's functions,
as well as modifications in it's basic fundamental properties. A
progressive growth of the Sun's general activity has been observed.
This growth revealed itself most definitely; which posed a real problem
for heliophysicists who were attempting to revise their main
explanatory scenarios:
Concerning the velocity of reaching super-flash maximums. Concerning
the emissive power of separate flashes. Concerning the energy of solar
cosmic rays, etc. Moreover, the Ulysses spacecraft, traversing high
heliospheric latitudes, recorded the absence of the magnetic dipole,
which drastically changed the general model of heliomagnetism, and
further complicated the magnetologist's analytic presentations. The
most important heliospheric role of coronal holes has now become clear;
to regulate the magnetic saturation of interplanetary space.
Additionally, they generate all large geomagnetic storms, and
ejection's with a southerly directed magnetic field are geo-effective;
an increase in the frequency of super-flashes. Jupiter is
having the possibility of being shrouded by a plasmosphere extending
over Io's orbit.
As a whole, all of the reporting and observation facilities give
evidence to a growth in the velocity, quality, quantity, and energetic
power of our Solar System's Heliospheric processes
1/8/98:
The unexpected high level of Sun activity, a 300% increase... The
character, scale, and magnitude of current Sun activity has increased
to the point that one official government Sun satellite reporting
station recently began their daily report by saying, "Everything pretty
much blew apart on the Sun today, Jan. 3,1998."
http://www.tmgnow.com/
http://www.tmgnow.com/
http://www.planetophysical2.html
Magnetic
Portals Connect Sun
and Earth
(this
article is on Universal
Life's Events and this link too and it is important
for understanding why we
all need to use the Sun's White Light Beam to move together with Earth
to the 5th Density. How to use this Beam? Just your Intent and constant
thoughts about it would be sufficient, LM).
"...Researchers have
long known that the Earth and sun must be connected.
(Sun is the Higher
Self of
Earth, in other words, our Earth and our Sun are the same thing. Did
you notice that often the word "Earth" would start from capital letter,
but not the word "sun", this way making our Sun less significant than
Earth, when in reality it should be the opposite, LM).
Earth's magnetosphere (the magnetic bubble that surrounds our planet)
is filled with particles from the sun that arrive via the solar wind
and penetrate the planet's magnetic defenses. They enter by following
magnetic field lines that can be traced from terra firma all the way
back to the sun's atmosphere.
We used to think the connection was permanent and that solar wind could
trickle into the near-Earth environment anytime the wind was active,"
says Sibeck. "We were wrong. The connections are not steady at all.
They are often brief, bursty and very dynamic..."
http://science.nasa.gov/headlines/y2008/30oct_ftes.htm
Spectral Colors
It is common practice to define pure colors in terms of the
wavelengths of light as shown. This works well for spectral colors but
it is found that many different combinations of light wavelengths can
produce the same perception of color.
This progression from left to right is from long wavelength to short
wavelength, and from low frequency to high frequency light. The
wavelengths are commonly expressed in nanometers (1 nm = 10-9 m). The
visible spectrum is roughly from 700 nm (red end) to 400 nm (violet
end). The letter I in the sequence above is for indigo - no longer
commonly used as a color name. It is included above strictly for the
reason of making the sequence easier to say as a mnemonic, like a
person's name: Roy G. Biv - a tradition in the discussion of color.
The inherently distinguishable characteristics of color are hue,
saturation, and brightness. Color measurement systems characterize
colors in various parameters which relate to hue, saturation, and
brightness. They include the subjective Munsell and Ostwald systems and
the quantitative CIE color system.
Introduction
The term light is usually taken to refer to visible light, the familiar
spectrum of red, orange, yellow, green, blue, violet. However, light
actually belongs to a much broader spectrum known as the
electromagnetic spectrum. It includes, in order of increasing
frequency, radio waves, infrared waves, visible light, Ultraviolet
rays, X rays, and Gamma Rays.
Electromagnetic Spectrum
The electromagnetic spectrum is the range of wavelengths and
frequencies that electromagnetic radiation can assume. This is a very
broad range, and these waves exhibit a variety of properties associated
with wavelength and frequency.
Long radio waves have the lowest frequency and wavelength - they
sometimes have frequencies less than 1 Hertz and wavelengths in excess
of 1 kilometer. They are generally used for long-range radio
transmissions. Short radio waves have higher frequencies and
correspondingly shorter wavelength; they are used mostly in very
short-range radio transmissions. AM (amplitude modulation) radio waves
have frequencies between these two wave types. In varying AM waves, the
strength or height (maximum displacement from equilibrium) is changed.
By contrast, FM (frequency modulation) radio waves usually have higher
frequencies closer to those of TV transmissions. In varying FM waves,
the frequency of the wave is changed. Exposure to radio waves causes no
major health problems and is not regulated.
Microwaves are higher-frequency waves lying roughly between radio and
infrared waves. They have a number of common applications, the most
familiar of which is the microwave or microwave oven used for cooking.
In these kitchen devices, microwaves are used to excite the water
molecules in food, thus generating heat. Microwaves can easily
penetrate nonmetal containers but generally cannot penetrate metal. For
this reason, food to be microwaved cannot be heated in metal
containers. High densities of microwave radiation (such as what is
found in masers, or "microwave lasers") are known to cause health
problems such as burns, cataracts, nervous-system damage, and
sterility. Exposure to microwave radiation is usually regulated; the
U.S. government limits exposure to 10 milliwatts per square centimeter
or less.
Infrared radiation is the portion of the electromagnetic spectrum just
below red light in terms of frequency. Infrared radiation, along with
visible light and ultraviolet rays, are produced by the transitions of
outer electrons. Infrared radiation has many applications in the field
of astronomy because earth's atmosphere does not scatter it as much as
visible light. Thus, special filters that block all but infrared rays
can be used to obtain precise astronomical images without the
scattering associated with visible light. Infrared radiation can also
be used in detecting the positions of objects or people in the absence
of visible light. This property has been put to good use in modern
military technology. A more mundane use of infrared light can be found
in the admissions booths of many theme parks, where visitors' hands are
stamped with special ink visible only under infrared lights to prove
that admission fees have been paid. A special infrared light, often
referred to as a black light, is used to detect the ink. Infrared
radiation itself is also often called "black light." Few if any
dangerous side effects result from low-level exposure to infrared
radiation.
Visible light is what is generally referred to by the term "light."
This is the only type of electromagnetic radiation detectable by human
eyesight. White light can be broken up into six distinct colors, each
corresponding to a separate frequency and wavelength. These colors are,
in order of increasing frequency, red, orange, yellow, green, blue,
violet.
(Indigo is often considered the seventh color of the spectrum, but is
no longer recognized as a distinct spectral color.) That's too bad
because it is!
This spectrum can be obtained by passing white light through a prism;
when it occurs naturally as a result of light reflection in water
droplets, it is called a rainbow. The colors seen in everyday life are
due to the disproportionate absorption of certain wavelengths by
everyday objects. For example, if an object is green, it tends to
absorb red, orange, yellow, blue, and violet light, but reflects green
light back to the observer. If an object is a color "in between" two
spectral colors - i.e., teal - then it reflects these two colors while
absorbing the others. In the case of teal (aquamarine), red, orange,
yellow, and violet light is absorbed, while green and blue light is
reflected. Aside from its ordinary applications, visible light spectrum
can be used to detect such things as changes in the configurations of
molecules.
Ultraviolet
light is just beyond violet light in terms of frequency. Its main
natural source is the sun and other stars; artificially, it is produced
by electric-arc lamps for scientific purposes. Ultraviolet rays are
often harmful to plants and animals, including humans
(to physical bodies yes, but very beneficial to the Soul: it raises Consciousness of a human/animal and plant! LM).
Their
danger is generally proportional to their wavelength. They are divided
into three categories: UV-A, UV-B, and UV-C. UV-A has the longest
wavelength and is least dangerous; UV-B is of intermediate wavelength
and is the type of sun emission that causes sunburn and, over long
periods of exposure, skin cancer; UV-C has a very short wavelength and
kills bacteria and viruses so well that it is often used to sterilize
surfaces. The earth's atmosphere, especially the ozone layer, provides
some protection from harmful UV rays from the sun; however, the
depletion of the ozone layer in recent years has led to an increase in
the amount of ultraviolet radiation to which the average human is
exposed. Also, ultraviolet radiation is not entirely harmful because
vitamin D is produced when it hits a human's or animal's skin. Another
interesting property of ultraviolet light is the fact that it causes
some objects to glow, or become fluorescent, upon contact. Molecules in
the object gain energy on contact with ultraviolet light, then release
the energy in the form of visible light. In astronomy, satellite-based
ultraviolet ray detectors provide excellent data on distant stars.
X rays, also known as Roentgen rays in honor of their discoverer, are
divided into two categories: soft and hard X rays. Soft X rays have
longer wavelengths and are closer to the ultraviolet band of the
spectrum. Hard X rays are closer to the gamma-ray band of the spectrum
and have much shorter wavelengths. X rays are produced when
high-velocity electrons are hit by material objects. Each element has a
certain spectrum of characteristic X rays associated with it that
identify it absolutely. This is extremely useful when studying the
elemental makeup of distant objects. X rays are highly penetrating of
ordinary objects, and their penetration power depends on the density
and atomic weight of the object. They find their best-known use in
medicine, where they easily penetrate flesh and are more effectively
absorbed by bone. The result is that bone appears white on a
photographic plate, while soft tissues appear gray. Another related,
familiar application of X rays is luggage scanning at airports and
other such facilities. Again, the empty portions of luggage or light
objects like clothing are easily penetrated by X rays, while other,
harder objects made of metal or hard plastic absorb the radiation more
effectively. X rays are also associated with ionization and research
into quantum mechanics; more information on these topics is available
in Theoretical Cosmology.
Gamma
rays are the shortest-wavelength, highest-frequency type of
electromagnetic radiation. They are essentially identical to X rays in
their effect, but are produced by excited nuclei instead of inner
electrons. They are the most penetrating of all electromagnetic
radiation. They are often produced as a result of gamma decay of
radioactive elements; this is the most dangerous and the most
penetrating of all radioactive decay.
Ultraviolet
The
region just below the visible in wavelength is called the near
ultraviolet. It is absorbed very strongly by most solid substances, and
even absorbed appreciably by air. The shorter wavelengths reach the
ionization energy for many molecules, so the far ultraviolet has some
of the dangers attendent to other ionizing radiation. The tissue
effects of ultraviolet include sunburn, but can have some therapeutic
effects as well.
The sun is a strong source of ultraviolet radiation, but atmospheric
absorption eliminates most of the shorter wavelengths. The eyes are
quite susceptible to damage from ultraviolet radiation. Welders must
wear protective eye shields because of the uv content of welding arcs
can inflame the eyes. Snow-blindness is another example of uv
inflamation; the snow reflects uv while most other substances absorb it
strongly.
Frequencies: 7.5 x 1014 - 3 x 1016 Hz
Wavelengths: 400 nm - 10 nm
Quantum energies: 3.1 - 124 eV
X-Rays
X-ray was the name given to the highly penetrating rays which emanated
when high energy electrons struck a metal target. Within a short time
of their discovery, they were being used in medical facilities to image
broken bones. We now know that they are high frequency electromagnetic
rays which are produced when the electrons are suddenly decelerated -
these rays are called bremsstrahlung radiation, or "braking radiation".
X-rays are also produced when electrons make transitions between lower
atomic energy levels in heavy elements. X-rays produced in this way
have have definite energies just like other line spectra from atomic
electrons. They are called characteristic x-rays since they have
energies determined by the atomic energy levels.
In interactions with matter, x-rays are ionizing radiation and produce
physiological effects which are not observed with any exposure of
non-ionizing radiation, such as the risk of mutations or cancer in
tissue.
Astronomical observations in the X-ray region of the spectrum are obtained with the Chandra X-ray Observatory.
X-rays are part of the Electromagnetic Spectrum
Frequencies: 3 x 1016 Hz upward
Wavelengths: 10 nm - > downward
Quantum energies: 124 eV -> upward
http://amazing-space.stsci.edu/glossary/def.php.s=topic_light
Absorption
The process by which light transfers its energy to matter. For example,
a gas cloud can absorb starlight that passes through it. After the
starlight passes through the cloud, dark lines called absorption lines
appear in the star’s continuous spectrum at wavelengths corresponding
to the light-absorbing elements.
Absorption Line
A dark line in a continuous spectrum caused by absorption of light.
Each chemical element emits and absorbs radiated energy at specific
wavelengths, making it possible to identify the elements present in the
atmosphere of a star or other celestial body by analyzing which
absorption lines are present.
Blueshift
The shortening of a light wave from an object moving toward an
observer. For example, when a star is traveling toward Earth, its light
appears bluer.
Color
The visual perception of light that enables human eyes to differentiate
between wavelengths of the visible spectrum, with the longest
wavelengths appearing red and the shortest appearing blue or violet.
Cosmic Rays
High-energy atomic particles that travel through space at speeds close
to the speed of light; also known as cosmic-ray particles.
Doppler Effect
The change in the wavelength of sound or light waves caused when the
object emitting the waves moves toward or away from the observer; also
called Doppler Shift. In sound, the Doppler Effect causes a shift in
sound frequency or pitch (for example, the change in pitch noted as an
ambulance passes). In light, an object’s visible color is altered and
its spectrum is shifted toward the blue region of the spectrum for
objects moving toward the observer and toward the red for objects
moving away.
Electromagnetic Radiation
A form of energy that propagates through space as vibrations of
electric and magnetic fields; also called radiation or light. All
electromagnetic radiation is a form of light.
Electromagnetic Spectrum
The entire range of wavelengths of electromagnetic radiation, including
radio waves, microwaves, infrared light, visible light, ultraviolet
light, X-rays, and gamma rays.
Emission Line
A bright line in a spectrum caused by emission of light. Each chemical
element emits and absorbs radiated energy at specific wavelengths. The
collection of emission lines in a spectrum corresponds to the chemical
elements contained in a celestial object.
Far-Infrared Spectrum
The region of the infrared spectrum that exhibits the longest wavelengths and the lowest frequencies and energies.
Frequency
Describes the number of wave crests passing by a fixed point in a given
time period (usually one second). Frequency is measured in Hertz (Hz).
One of
the most energetic gamma-ray bursts (GRBs) ever detected, occurring at
4:47 a.m. EST, January 23, 1999. The “burst” equaled the power of
nearly 10 million billion suns. It became the first GRB to be viewed
simultaneously in both gamma-ray and optical wavelengths.
Gamma-Ray Burst (GRB)
A brief, intense, and powerful burst of gamma rays, the
highest-energy, shortest-wavelength radiation in the electromagnetic
spectrum. These bursts emanate from distant sources outside our galaxy
and last only a few seconds. They are the brightest and most energetic
explosions known.
Gamma Rays
The part of the electromagnetic spectrum with the highest energy; also called gamma radiation.
Gravitational Redshift
The reddening of light from a very massive object caused by photons
escaping and traveling away from the object’s strong gravitational
field. An example of gravitational redshift is light escaping from the
surface of a neutron star.
Infrared
Radiation that has longer wavelengths and lower frequencies and energies than visible light.
Invisible Radiation
Radiation that the eye cannot detect, such as gamma rays, radio waves, ultraviolet light, and X-rays.
Near-Infrared
The region of the infrared spectrum that is closest to visible light.
Near-infrared light has slightly longer wavelengths and slightly lower
frequencies and energies than visible light.
Radiation
The process by which electromagnetic energy moves through space as
vibrations in electric and magnetic fields. This term also refers to
radiant energy and other forms of electromagnetic radiation, such as
gamma rays and X-rays.
Radio Waves
The part of the electromagnetic spectrum with the lowest energy. Radio
waves are the easiest way to communicate information through the
atmosphere or outer space.
Redshift
The lengthening of a light wave from an object that is moving away from
an observer. For example, when a galaxy is traveling away from Earth,
its light shifts to the red end of the electromagnetic spectrum.
Spectral Line
In a spectrum, an emission (bright) or absorption (dark) at a specific frequency or wavelength.
Spectrograph (Spectrometer)
An instrument that spreads electromagnetic radiation into its component
frequencies and wavelengths for detailed study. A spectrograph is
similar to a prism, which spreads white light into a continuous rainbow.
Spectroscopy
The study and interpretation of a celestial object’s electromagnetic
spectrum. A spectrograph or spectrometer is used to analyze an object’s
electromagnetic spectrum.
Sprites
Gamma-ray flashes produced in Earth’s atmosphere by severe lightning storms and upper atmospheric events.
Ultraviolet (UV)
Electromagnetic radiation with shorter wavelengths and higher energies
and frequencies than visible light. UV light is lower in frequency than
X-rays.
Visible Light
The part of the electromagnetic spectrum that human eyes can detect;
also known as the visible spectrum. The colors of the rainbow make up
visible light. Blue light has more energy than red light.
Wave
A vibration in some media that transfers energy from one place to
another. Sound waves are vibrations passing in air. Light waves are
vibrations in electromagnetic fields.
Wavelength
The distance between two wave crests. Radio waves can have lengths of
several feet; the wavelengths of X-rays are roughly the size of atoms.
X-Rays
The part of the electromagnetic spectrum with energy between
ultraviolet light and gamma rays. X-rays are used in medicine to detect
broken bones and cavities in teeth. Astronomers can detect X-rays from
exploding stars and black holes.
Accretion Disk
A relatively flat, rapidly rotating disk of gas surrounding a black
hole, a newborn star, or any massive object that attracts and swallows
matter. Accretion disks around stars are expected to contain dust
particles and may show evidence of active planet formation. Beta
Pictoris is an example of a star known to have an accretion disk.
Binary Star System
A system of two stars orbiting around a common center of mass that are bound together by their mutual gravitational attraction.
Blue Star
A massive, hot star that appears blue in color. Spica in the constellation Virgo is an example of a blue star.
Brown Dwarf
An object too small to be an ordinary star because it cannot produce
enough energy by fusion in its core to compensate for the radiative
energy it loses from its surface. A brown dwarf has a mass less than
0.08 times that of the Sun.
Cepheid Variable
A type of pulsating star whose light and energy output vary noticeably
over a set period of time. The time period over which the star varies
is directly related to its light output or luminosity, making these
stars useful standard candles for measuring intergalactic distances.
Dark Dust Cloud
A region of interstellar space that contains a rich concentration of
gas and dust. Such a cloud is often irregular in shape but sometimes
has a well-defined edge. Visible light cannot pass through these
clouds, so they obscure the light from stars beyond them.
Gaseous Nebula
A glowing cloud of gas in interstellar space. The cloud of gas may be
either an emission nebula, which absorbs ultraviolet light from nearby
stars and re-radiates visible light, or a reflection nebula, which
reflects light off of its dust particles.
Giant Star
A dying star that has used up the hydrogen fuel in its core and has
begun to expand. Giant stars are generally larger than our Sun.
Globular Cluster
A collection of hundreds of thousands of old stars held together by
gravity. Globular clusters are usually spherically shaped and are often
found in the halos of galaxies. Each star belonging to a cluster
revolves around the cluster’s common center of mass.
Hertzsprung-Russell Diagram
A plot showing the relationship between the brightness (luminosity) and
the surface temperatures of many stars. Often the spectral class, which
is based on the temperature of the star, is used as a label.
Interstellar Dust
Small particles of solid matter, similar to smoke, in the space between stars.
Interstellar Medium (ISM)
The sparse gas and dust located between the stars of a galaxy.
Interstellar Space
The dark regions of space located between the stars.
Light Curve
A plot showing how the light output of a star (or other variable astronomical object) changes with time.
Molecular Cloud
A relatively dense, cold region of interstellar matter where hydrogen
gas is primarily in molecular form. Stars generally form in molecular
clouds. Molecular clouds appear as dark blotches in the sky because
they block all the light behind them.
Neutron Star
An extremely compact ball of neutrons created from the central core of
a star that collapsed under gravity during a supernova explosion.
Neutron stars are extremely dense: they are only 10 kilometers or so in
size, but have the mass of an average star (usually about 1.5 times
more massive than our Sun). A neutron star that regularly emits pulses
of radiation is known as a pulsar.
Nova
A binary star system (consisting of a white dwarf and a companion star)
that rapidly brightens, then slowly fades back to normal.
Period-Luminosity Law
A relationship that describes how the luminosity or absolute brightness
of a Cepheid variable star depends on the period of time over which
that brightness varies.
Planetary Nebula
An expanding shell of glowing gas expelled by a star late in its life.
Our Sun will create a planetary nebula at the end of its life.
Protostar
A collection of interstellar gas and dust whose gravitational pull is causing it to collapse on itself and form a star.
Pulsar
A neutron star that emits rapid and periodic pulses of radiation.
Red Giant Star
An old, bright star, much larger and cooler than the Sun. Betelgeuse (alpha Orionis) is an example of a red giant.
Spectral Class (Spectral Type)
A classification scheme that groups stars according to their surface temperatures and spectral features.
Spectral Line
In a spectrum, an emission (bright) or absorption (dark) at a specific frequency or wavelength.
Star
A huge ball of gas held together by gravity. The central core of a star
is extremely hot and produces energy. Some of this energy is released
as visible light, which makes the star glow. Stars come in different
sizes, colors, and temperatures. Our Sun, the center of our solar
system, is a yellow star of average temperature and size.
Star Cluster
A group of stars born at almost the same time and place, capable of
remaining together for billions of years because of their mutual
gravitational attraction.
Starburst Galaxy
A galaxy undergoing an extremely high rate of star formation. Starburst
galaxies contain massive, deeply embedded stars that are among the
youngest stars observed.
Stellar Evolution
The process of change that occurs during a star’s lifetime from its birth to its death.
Supernova
The explosive death of a massive star whose energy output causes its
expanding gases to glow brightly for weeks or months. A supernova
remnant is the glowing, expanding gaseous remains of a supernova
explosion.
Supernova Remnant
The glowing, expanding gaseous remains of a supernova explosion.
T-Tauri Star
A class of very young, flaring stars on the verge of becoming normal stars fueled by nuclear fusion.
Variable Star
A star whose luminosity (brightness) changes with time.
White Dwarf Star
The hot, compact remains of a low-mass star like our Sun that has
exhausted its sources of fuel for thermonuclear fusion. White dwarf
stars are generally about the size of the Earth
"Ancient Galaxy remotest object
observed"
http://bigpondnews.com/articles/Technology/2010/10/21/Ancient_galaxy_remotest_object_observed_528644.html
Thursday, October 21, 2010 » 04:40am
(This persistence is getting on my
nerves! There is a lot of misleading information in all these official
articles, because they are written by paid astronomers or even by
people, who has very little understanding of the events happening in
out Universe! They are like parrots will be repeating the nonsense
about "the light years" even after the physical Earth will be gone from
here and the Timeline for our physical Universe will come to 0, which
is not that far away! That I told M. Kushnir, the "lecturer" from
Israel at the Conference at the Centre for "Theoretical" (not real that is!) Physics
in Trieste, Italy! LM)
European astronomers say a galaxy born in the childhood of the
Universe lies at least 13 billion light years away, making it the
remotest object ever observed.
(Bullshit! How can they observe it
that far away if they still use linear measurements? This is possible
only if that Galaxy approached our Planet close enough and I wouldn't
be surprised if that really happened
as a result of the mixture of all the remaining Galaxies in our
Universe! Most of the Suns and Planets have left our Universe and that
is natural if our whole Universe is moving to the non-physical, higher
4th Level of Consciousness! LM)
Light from the galaxy UDFy-38135539 that reaches Earth today was
emitted when the cosmos was only 600 million years old and mired in a
primordial 'fog' of hydrogen atoms, they said on Wednesday.
It has taken 13.1 billion years, travelling at 300,000 kilometres per
second, for this smudge of infant light to arrive.
The study, appearing in the British journal Nature, used a giant
European telescope in Chile's Atacama desert to measure the galaxy's
so-called redshift.
The more distant a light source is, the longer its wavelength
stretches. In other words, a light that appears to be receding from the
observer shifts more towards the red part of the optical spectrum.
In this case, the galaxy's redshift was 8.6, making it the most distant
object ever observed by spectroscopy.
The previous documented record, in 2009, was a redshift of 8.2 caused
by a gamma-ray burst of a super-massive star. An object at a redshift
of 10 was once reported but has never been confirmed.
'Measuring the redshift of the most distant galaxy so far is very
exciting in itself, but the astrophysical implications of this
detection are even more important,' said Nicole Nesvadba of France's
Institut d'Astrophysique Spatiale.
'This is the first time we know for sure that we are looking at one of
the galaxies that cleared out the fog which had filled the very early
Universe.'
Under the Big Bang theory, the Universe originated in a
superheated-flash around 13.7 billion years ago and started to expand.
After the cosmos had cooled a little, electrons and protons teamed up
to form hydrogen, which for hundreds of millions of years filled the
Universe.
During this epoch, known as the Universe's Dark Ages, there were no
stars. It was followed by a period known as reionisation, in which the
first stars formed and their intense ultra-violet
radiation managed to pierce the hydrogen fog.
Understanding reionisation would also help to explain the formation of
the first galaxies. But the starlight needed for evidence has - until
now - been absent because of the opaque mist that shrouded the Universe
at this time.
One theory is that the light from the newly-discovered galaxy was able
to penetrate the fog because it was helped by other, nearby galaxies.
'Without this additional help, the light from the galaxy, no matter how
brilliant, would have been trapped in the surrounding hydrogen fog and
we would not have been able to detect it,' said astronomer Mark
Swinbank of Durham University, northeast England.
UDFy-38135539 - whose name comes from its location in the Ultra Deep
Field zone of deep space - was first spotted last year by the US
orbital telescope Hubble.
The dim light intrigued astronomers poring over the reionisation
enigma, said lead author Matt Lehnert of the Observatoire de Paris.
They begged the boss of the European Southern Observatory (ESO) to give
them special time on the Very Large Telescope (VLT), which has a highly
sensitive redshift-measuring spectroscope.
Sixteen hours of observation, using a very long exposure time, enabled
a clearer image of the galaxy, but two months of analysis and testing
were needed to confirm the data.
In terms of distance, the gap between Earth and the galaxy is likely to
be far higher than 13 billion light years, ESO told AFP.
This is because the Universe has been expanding since the time when the
light was first emitted
(and
now our Universe is shrinking as a result of the Transformation of the
Level of Consciousness in it to much higher Level! And again this
bullshit about "the light has had to travel longer in order to catch up
with us"! They stuck to the linear measurements for good and they want
us to think only in linear terms, not holographic ones! LM). As a
result, the light has had to travel longer in order to 'catch up' with
us."
