ne bom reku da ni tud ta varianta obstajala kot realnost trenutka
pa ne zdrži velik enih drugih faktov ki obstajajo ... ki so seveda lahko tud podtaknjeni - izmišljeni
nč ne rečem
lahko da je tko kot praviš
in mislm da se ne rabiš bat da bi kdo ne živel življenja ki je za živet
na konc pa se slisti zadeva na
naključje
ali
namen

za naključje, je nekoliko preveč naključij
obstaja namen

bomo vidl zadost hmal se mi zdi ...


pa veselo plavanje

david wilcock

Petra. wrote on 11.05.2012 at 14:19:51:

none doom & gloom

Venus Transit of 2012 - Not Seen Again Unil 2117

By Earth Changes Media
May 4, 2012 - 10:28:47 PM
     


The next transit of Venus will occur on June 6th (Tuesday, June 5th from the Western Hemisphere) in 2012. After 2012, the next transits of Venus will be in December 2117 and December 2125. The entire event will be widely visible from the western Pacific, eastern Asia and eastern Australia. Most of North and Central America, and northern South America will witness the beginning of the transit (on June 5) but the Sun will set before the event ends. Similarly, observers in Europe, western and central Asia, eastern Africa and western Australia will see the end of the event since the transit will already be in progress at sunrise from those locations.

For Northern Hemisphere locations above latitude ~67° north, all of the transit is visible regardless of the longitude. Northern Canada and all of Alaska will also see the entire event. Residents of Iceland are in a unique wedge-shaped part of the path. They will see both the start and end of the transit but the Sun will set for a short period around greatest transit. A similarly shaped region exists south of Australia, but here, the Sun rises after the transit begins and sets before the event ends.

The principal events occurring during a transit are conveniently characterized by contacts, analogous to the contacts of an annular solar eclipse. The transit begins with contact 1, the instant the planet's disk is externally tangent to the Sun. Shortly after contact I, the planet can be seen as a small notch along the solar limb. The entire disk of the planet is first seen at contact 2 when the planet is internally tangent to the Sun. Over the course of several hours, the silhouetted planet slowly traverses the solar disk. At contact 3, the planet reaches the opposite limb and once again is internally tangent to the Sun. Finally, the transit ends at contact 4 when the planet's limb is externally tangent to the Sun. Contacts 1 and 2 define the phase called ingress while contacts 3 and 4 are known as egress. Position angles for Venus at each contact are measured counterclockwise from the north point on the Sun's disk.

During the 2012 transit, Venus's minimum separation from the Sun is 554 arc-seconds (During the 2004 transit, the minimum separation was 627 arc-seconds). The position angle is defined as the direction of Venus with respect to the center of the Sun's disk, measured counterclockwise from the celestial north point on the Sun. Figure 2 shows the path of Venus across the Sun's disk and the scale gives the Universal Time of Venus's position at any point during the transit. The celestial coordinates of the Sun and Venus are provided at greatest transit as well as the times of the major contacts.

Note that these times are for an observer at Earth's center. The actual contact times for any given observer may differ by up to ±7 minutes. This is due to effects of parallax since Venus's 58 arc-second diameter disk may be shifted up to 30 arc-seconds from its geocentric coordinates depending on the observer's exact position on Earth.

Observing the Transit

Since the apparent diameter of Venus is nearly 1 arc-minute, it is just possible to see without optical magnification (but using solar filter protection) as it crosses the Sun. Nevertheless, the planet appears to be only 1/32 of the Sun's apparent diameter so a pair of binoculars or a small telescope at modest power will offer a much more satisfying view. All binoculars and telescopes must be suitably equipped with adequate filtration to ensure safe solar viewing. The visual and photographic requirements for observing a transit are identical to those for solar viewing. Amateurs can make a scientific contribution by timing the four contacts at ingress and egress. Observing techniques and equipment are similar to those used for lunar occultations. Poor seeing often increases the uncertainty in contact timings, so an estimate of the possible error associated with each timing should be included.

Frequency of Transits

The orbit of Venus is inclined 3.4° with respect to Earth's orbit. It intersects the ecliptic at two points or nodes that cross the Sun each year during early June and December. If Venus happens to pass through inferior conjunction at that time, a transit will occur. Although Venus's orbital period is only 224.7 days, its synodic period (conjunction to conjunction) is 583.9 days. Due to its inclination, most inferior conjunctions of Venus do not result in a transit because the planet passes too far above or below the ecliptic and does not cross the face of the Sun. Venus transits currently recur at intervals of 8, 105.5, 8 and 121.5 years. Since the invention of the telescope (1610), there have only been seven transits as listed.


Transits of Venus: 1601-2200

Date                  Universal Time      Separation

1631 Dec 07         05:19                     939 "
1639 Dec 04        18:26                      524 "
1761 Jun 06         05:19                      570 "
1769 Jun 03         22:25                      609 "
1874 Dec 09        04:07                       830 "
1882 Dec 06        17:06                       637 "
2004 Jun 08        08:20                        627 "
2012 Jun 06        01:28                        553 "
2117 Dec 11        02:48                        724 "
2125 Dec 08        16:01                        733 "

The 2004 and 2012 transits form a contemporary pair separated by 8 years. More than a century will elapse before the next pair of transits in 2117 and 2125. During the 6,000-year period from 2000 BC to AD 4000, a total of 81 transits of Venus occur.

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