DE3726534A1 - Electronic solar globe - Google Patents

Abstract

The electronic solar globe is a three-dimensional precision instrument which can be rotated and inclined in any direction and realistically reproduces over 20000 eclipses in a period of 10000 years. Solar globe with eclipse phases, protruberances, string-of-pearl phenomena and corona. Course of eclipse in REAL TIME with advancing date and time announcement, refered to world time or dynamic time. Starting from the date input, the next 22 eclipses may be chosen. The entire course of the eclipse region and zone of totality is reproduced on the terrestrial globe (with day/night side and twilight zone), the world map and fundamental plane, with migrating umbras and penumbras of the moon. Accuracy of the solar and lunar position: 1 arc second. All technical and physical data can be called up using panels which can be switched over in each case; data such as geographical longitude and latitude of the central line, eclipse duration etc. Solar rotation with sporadically occurring sun spots. In addition: grids of parallels and meridians, city names which can be called up, 4 enlargements and two extensions of the celestial segment with stars and planets (inform. by means of switching on) and reproduction of all the passes of mercury and venus. The space globe is self-explanatory. The accompanying text contains historical solar eclipses, which can be reproduced by inputting date and time, as well as extensive explanations of the production of the eclipses, sun spots and more.

Description

The electronic sun globe is a three-dimensional, rotating and inclinable precision instrument. Over 10 000 years shows the Globe, in reduced dimension, in REAL TIME PROGRAM with continuous Date and time, from 1.1.5001 v. To 31.12.4999 AD, over 20 000 eclipses.

After entering the date and time, the eclipse process on the Sunglobe, in real time (running time display), with Eclipse phase, corona, pearl cord phenomenon and protuberances, played. Real-time process also on the Earth globe with Day / night time, twilight zone and retrievable city names. The globe circuit tilts and turns the sun or earth globe in every direction.

Additionally selectable: different graticules, four magnifications (Telescope) and two extensions of the sky section - also each with a continuous date and time. The Detail shows planets and stars near the apparent Solar orbit (ecliptic). Inform. To the planets, stars and Phenomena, each with switchable panels.

From date input the next 22 eclipses are available. The whole process will be at the solar, earth globe, world map and Fundamental level reproduced (optionally switchable), as well the wandering core and partial shade of the moon on the Fundamental level, specifying the darkness elements. The SPACEGLOBE is self-explanatory.  

All technical and physical data in tabular form, as geogr. Length and width of the center line, limit, width in kilometers, total duration, central meridian, axial position, ecliptic, equatorial and horizontal coordinates, etc. Accuracy of sun and moon position: 1 arcsec. Solar rotation with sporadically occurring sunspots. Rendering of all Mercury and Venus passages in front of the Sun for 10 000 years, including the data.

The color of the sky is the respective sun and Darkness level adjusted.

Time entry in world or dynamic time.

After entering the date, the buttons A / K / D are available. World time input: Key <A <with automatic internal calculation of the correction value Δ T to 1 minute minute exactly. The zone time differs 1 hour from the world time. To obtain world time, subtract 1 hour from the Central European Time (CET) (World Time = CET minus 1 hour, Summer Time: World Time = CET minus 2 hours).

Key <K <to enter the world time and the respective correction value Δ T , according to table S., for arc and time-second accuracy. All times are based on world time.

The correction value Δ T is the difference between the constant and uniform artificial dynamic time (TDT) and the nonuniform, irregular world time (UT) . Key <D <: Entering Dynamic Time, omitting Δ T (p.), So that all times are Dynamic Times.

Date, time and geogr. input Date: 1.4.1982 (key <K <) time: 12 (12 o'clock UT Δ T Tab. S.) Geogr. Width: 50 Geogr. Length: 7 Place name: Frankfurt / M. Height above sea level in meters: 200

Complete each entry with the return or enter key

Geogr. Longitude, latitude and altitude above sea level, according to a world or topographic map. ( Fig. 1)

The sun

In the sun's interior temperatures are up to 20 million Degrees, while the surface temperature is about 6000 degrees. The pressure is some 100 billion at, the mass loss through Radiation per second about 4.3 billion kg, while losing the Sun in 10 billion years with constant luminosity only 0.1% of its mass (1.9891 · 10³⁰ kg). In 5 billion years are only about 2% consumed, so that still several 10 billion years undisturbed Energy is broadcast to the same extent.

Energy and luminosity arise largely through atomic Core processes, where 4 hydrogen atoms to form a helium atom be merged - it creates only a small amount of energy, but by size and number of core processes results in one Total transmission of 5.2 · 10²³ PS / sec.

The sun has a clearly visible demarcation, in the Matter density and gas pressure within 500 km fall to zero values and which is considered a solar surface.  

The gas bubbles bubbling up to millions become Called granules. Its mean diameter is 700 km, the Life time at 8 min. The granulation is due to hotter and brighter ascending, cooler towards, flowing off Matter. Near the edge of the sun become higher and cooler gases observed (marginal obscuration) while in the midst of the solar disk deeper and hotter layers are therefore essential appear lighter.

With the naked eye we see the dazzlingly bright photosphere (Light envelope), which is their outer light or mirror gloss layer forms. This light gloss layer reaches up to 500 km altitude. The high light intensity is not due to sole nuclear fusion to explain. As a result of their significant size, the light becomes countless stars on the spherical light luster layer of the Photoacid, according to the optical laws of light reflection magnified and mirrored.

We see a bright but small solar disk (1 penny piece in 1.8 m corresponds to its apparent angular diameter [0 ° 31'59 '']). Because of its long distance (1,496 million km), we see the 1,392,000 km sun only at this small angle (0.533127 ° · 149 600 000 km = 1 392 000 km). On the sunniest planet Mercury it seems to be increasing. Angle diameter to 1 ° 44 '(1 Pfennigstück in 0.5 m distance). With 1.4 g cm³ corresponds to their average. Density of the giant planets Jupiter, Saturn and Uranus. Gravitational acceleration 274 ms ^-2 (28 times the earth's gravity). Speed to maintain a circular path 437 km / sec. · √ = escape speed 618 km / sec. (Earth 11 km / sec.). 109 earth balls make up the sun diameter. Volume of the Sun 1,412 · 10¹⁸ km³ (Earth 1083.32 · 10⁹ km³).

On the surface there are huge discharges and gas eruptions instead, the gases (protuberances) at 700 km / sec. flung up to 2 million km altitude. Not on the sun Falling remnant causes magnetic interference terrestrial ionosphere (influences the radio traffic), causes polar lights, etc. Connections between periods of drought and solar activity could be detected.  

The sunspots were discovered telescopically in 1610, but larger ones were observed much earlier by the naked eye - they are the eruptive volcanoes of the sun ( Fig. 29 and Fig. 30). The ejected matter can be observed with special telescopes (coronographs), or at total solar eclipses as protuberance, at the edge of the sun. These are matter bales or vortexes which, as a result of solar rotation and strong centrifugal acceleration, can break through the plastic solar surface, similar to terrestrial volcanoes. The centrifugal acceleration is maximally effective in the equatorial region, so that the sunspots occur mainly there, seldom between ± 40 ° and ± 50 ° heliocentric latitude, never above.

The funnel-shaped opening of the sunspots (umbra) appears pitch black, because the surface breakthrough only 500 km high Light envelope is torn. The raised wall (Penumbra) is brighter, as this upward-expanded ball due to vibrations is stimulated to self-lighting. The changed direction angle the funnel, its height or depth position opposite the Wallform, is known as the Schulen-Wilson phenomenon.

The plastic property of the solar surface, which strives is to close the resulting opening funnel leads to the fast flowing changes of the sunspots. The dark spots are with bright light veins so-called sun torches surrounding the observer due to the marginal obscuration, however only near the edge of the sun, becoming more visible. These Sun flares are the result of the breakthrough Waves of the photosphere.

The pharmacist and amateur astronomer Heinrich Schwabe (1789-1875) discovered systematically at his since 1846 Sun observations the eleven-year sunspot period. To At the minimum, the first spots appear at the beginning of a new one Cycle between ± 30 ° and ± 45 ° heliogr. Width. With progressing Cycle approaches the activity zone Solar equator. While near the equator, the stains of the old Cycle pass, the new starts in higher latitudes Spot activity. In Max. They occur at ± 16 ° width.  

The ejected matter is subject to gravitation and the magnetic force fields of the sun, so that the Protuberances along the field lines, back to the surface decline.

Sunspots usually occur in pairs or bipolar, the one spot the magnetic 'North Pole', the other the 'South Pole' forms. Z. zt. Of the maximum of the stain activity, is reversed the relationship around: that towards the solar rotation pre-migratory, previously negative spot is then the positive. The magnetic properties of the Northern Hemisphere are always vice versa to those of the southern hemisphere and also change with the eleven-year rhythm of stain activity, so that the Total activity takes 22 years.

Because of the gaseous surface texture is no Reference point present from which counted the heliocentric length can be. The central meridian on 1 January 1854 12 o'clock DT, is hence the internationally established zero meridian. Of this so-called Carrington's central meridian becomes the heliographic one Length (0 ° .. 360 °) counted to the west. After expiration of a Synodic rotation (average 27.275 days) it forms again the central meridian. The Carrington solar rotation therefore starts at 0 degrees heliogr. Length (ZM = 0 °). Carrington introduced a numbering of this rotation. At the 17.1.1996 begins the rotation no. 1905 (Zm = 0 °), on 13.2.1996 No. 1906 etc.

The differential solar rotation discovered Richard Carrington 1863. The sun then does not rotate like a rigid body - the rotation time is maximal at the equator (synodically 26.9 days, siderisch 25.03 days) and with increasing heliogr. width decreasing. When observing higher or lower layers of the Surface are also different. rotation times determine. The determination of the central meridian after Carrington applies to ± 16 ° heliogr. Width (sider 25.38 days, syndically 27,275 days), as most sunspots to be observed there.  

eclipses

If the moon were farther away or its apparent diameter much smaller, could total solar eclipses not arise - it would always be a more or less wider Radiant ring visible around the dark moon. Not only, that the moon in relation to the earth size and mass as "Doppelplanet" would have to be classified (all other moons in the Solar system are tiny in relation to the planetary diameter), we have, the impressive natural spectacle of a total Solar Eclipse, this unique size and distance ratio Thanks to the sun-earth moon. The sun is indeed 400 times farther away, but also 400 times larger, so that both have approximately the same apparent angular diameter. As a result of this cosmic precision, the total arises Covering the sun.

The first solar eclipse noted in Germany dates back to the Metz manuscript 538 AD

Emperor Ludwig I, the pious, died on 20.6.840 Ingelheim / Rhein in shock over a falling in Eclipse.

The earliest surviving solar eclipse was 4100 years ago. In ancient China, the people believed in a solar eclipse devour a dragon the sun, only through much noise, Howls, bangs and trumpets, could be scared away, it had to He is so scared that he will restore the sun spat. For the warnings of such terrible events were the court astronomers Hi and Ho responsible, which, however, after the report of the Chung K'ang Chronicle, which indulged drunkenness and neglected about the calendar, so that the dragon without Previous countermeasures to devour the sun forever threatened. Hi and Ho were executed in public.

Date: 22.10.-2136 (key <D <) time: 15:25:18 (15:25 min 18 seconds) Geogr. Width: 18.0724 (18 ° 7'24 '' north lat. Br.) Dyn length: -53.1130 (-53 ° 22'30 '' dynamic length) Place name: - Height NN: 0 Key <F <.

The Eclipse of July 31, 1063 BC Was from the Babylonians recorded. The cuneiform script reads: "On the 26th day of the Month Sivan in the 7th year became the day to night and fire originated."

Date: 31.7.-1062 (key <D <) time: 11.4218 Geogr. Width: 30.5548 Dyn length: 4.3348 Place name: - Height NN: 0 Key <F <.

The Dark of 6.4.648 BC BC is from the Greek poet Archiochos mentions: "Do not swear the impossible, wonder nothing since Zeus made noon at night, the sunbeams hide and woe fear seized man. "

Date: 6.4.-647 (key <D <) time: 13.3648 Geogr. Width: 50.5724 Dyn length: -23.2854 Place name: - Height NN: 100 Key <F <.

Date, dynamic time and place for the eclipse center

The records of old chroniclers contain many references on spectacular eclipses, especially the historians enable accurate data of important historical events to determine. So it was known that at the beginning of the 6th century a Battle between Lydians and Medes under their kings Alyattes and Cyaxares broke out. A chronicler of antiquity reports (Herodot 1:74): "War was between Lydians and Medes erupted and raged for 5 years with varying degrees of success. , , when during a fight in the 6th year, the fierce battle fiercely growth, the day suddenly became night. , . "  

This is the darkness of 28.5.585 v. Chr. Chr., so that the date of the battle is fixed. After entering the natural spectacle predicted by Thales from Miletus, a tremendous howl of terror began among the mercenaries whereupon they even left all fight and peace closed together.

Date: 28.5.-584 (key <D <) time: 19.0112 Geogr. Width: 39.5324 Dyn length: -107.38 Place name: - Height NN: 0 Key <F <.

The darkness of 30.4.463 BC Chr. Described the greek. Poet Pindar: "Oh sunbeam, you look far, what will You think? Oh, the highest of the stars, which you see us in the light of You are snatched off today! Why do you have the power of man and the paths of wisdom are confused by going now in dark ways forteilst? God can turn the pure light of the day into a dark one Envelop cloud. "

Date: 30.4.-462 (key <D <) time: 16.0748 Geogr. Width: 34.45 Dyn length: -63.1948 Place name: - Height NN: 0

Darkness of the poet and chronicler Thucydides dated 3.8.431 v. "At the beginning of a lunar month in the afternoon was the The sun darkened and some stars became visible. "

Date: 3.8.-430 (key <D <) time: 18.1254 Geogr. Width: 83.3254 Dyn length: -92.4106 Place name: - Height NN: 0

Agathocles, fleet commander from Syracuse, was on 15.8.310 v. Surprised by an eclipse in front of Africa's north coast, where he was at war with the Carthaginians (Diodor 20.5): "The next Days an eclipse occurred at the many stars became visible. "

Date: 15.8.-309 (key <D <) time: 11.1906 Geogr. Width: 36.1436 Dyn length: 10.4548 Place name: - Height NN: 0

Darkness of Hipparch 20.11.129 BC In Alexandria were " 4/5 (80%) of the sun eclipses, while in the Hellespont total was. "

Date: 20.11.-128 (key <D <) time: 15.3424 Geogr. Width: 37.33 Dyn length: -56.2148 Place name: - Height NN: 0

The Austrian painter and poet Adalbert Stifter experienced in Vienna the solar eclipse of 8.7.1842: "There are things that one knows for fifty years, and in the fifty-first one one is astonished about the severity and the tractability of their contents. That's how it is for me with the total solar eclipse, which we in Vienna on 8.7.1842 in the early morning with a favorable sky experienced. - Never in my life have I been so shaken of chill and grandeur as in the two minutes, it was not differently, as if God suddenly had a clear word spoken and I would have understood it. "

Date: 8.7.1842 (key <D <) time: 6.5530 Geogr. Width: 51.4436 Dyn length: 77.1642 Place name: - Height NN: 0

The moon's orbital plane is opposite the earth's orbital plane (ecliptic) Tilted 5 °, so that eclipses only at new moon (sun-moon Earth in a line) and near one of the two intersections (Moon / earth orbit) can enter (ecliptic width of the moon near 0 °). At max. ekl. It can be up to 10 times its width Diameter north or south of the sun pass over. Reached the moon at new moon the ascending or descending node of his Train (dragon head and dragon tail with the Chinese), it must inevitably come to a cover (ekl. width of the sun always 0 °).

The lunar nodes move westward a bit every day and need for a round 18.6 years. As the knot of the sun she only needed 346.62 days to get back to reach the same node. The moon reaches average every 29.5306 days the same phase (new moon). An eclipse can therefore only arise if a multiple of 29.5306, the same of 346.62, which is after 223 new moons and 19 times the passage the sun is almost reached through the lunar knot.

Saros:
29.5306 · 223 = 6585.32 days
346.62 · 19 = 6585.78 days.

For this reason, the same darkness can only after expiration a saros period (6585.32 days or 18 years 11.3 days [at 4 leap years] or 18 years 10.3 days [at 5 leap years]) to repeat. At integer ratio would be the Eclipse again in the same place. Since the saros period a full Number of days and 1/3 day, the earth turned 360 ° times 0.3 days = 120 degrees further, so that the same darkness after 18 years 11.3 days for a 120 ° west Earth location repeated. But there are several such periods side by side, therefore occur within a year several Eclipses. A saros period with a saros gap goes after about 12 to 15 centuries into another Saros cycle over.  

During the passage, by the ascending or descending Moon knot, arise several eclipses, then again after a 1/2 year, passing the other node. At least 2 solar eclipses must occur per year. A total darkness is limited to constantly changing places. For one and the same place a total darkness is a rare one Event that occurs only once every 200 years.

The end of the moon's core shadow cone is called the central line, which reaches to the ground during a solar eclipse ( Figure 2). This totality zone, with northern and southern limits of the shadow cone, can be about 300 km wide. Because of lunar movement and rotation of the earth, this core shadow cone sweeps across the earth's surface at 2100 km / h. The totality at which the moon covers 100% of the sun does not last longer than 7.6 min at the equator (maximum 6.5 min at 45 ° latitude).

From the plane or a hill and at very narrow Sun-sickle, about 1 minute before and after the totality, that is scary-looking approach of so-called "flying shadows" to notice - dark stripes about 4 to 5 per square meter. These streaks of air move at about 1 km / sec. on the Ground.

The extent of the eclipse-limited eclipse area comprises several 1000 km ( FIG. 2). The coverage is determined by the location within the Eclipse area.

If the angular diameter of the moon is slightly larger than that of the sun, the darkness is total (<100%). Reach the core shadow cone straight down to the ground (solar and lunar diameters are equal), the totality duration shrinks to a moment together (t), the so-called bead-string phenomenon occurs, whereupon already in 1715 Halley and 1737 MacLaurin pointed out and by F. Bailey 1836 was described in more detail (in English therefore also "Baily's beards ").  

The so-called bead-string phenomenon, which then appears, arises as a result of the moon profile. The sunlight can still through the valleys and The mountains of the rugged lunar edge radiate in the sky into many, like diamonds sparkling points of light dissolved appears.

Is that sham? Angle diameter of the sun slightly larger than that of the moon, the eclipse is annular (<98%). A Darkness can first become ring-shaped, then totally "rt". A annular solar eclipse takes max. 12.4 minutes.

If only the moon half-shadow falls on a part of the earth, strike the core shadow cone of the moon so north or south to the Earth poles can pass, only partially or partially Eclipses arise.

Gen. Name of the darkness Total, central darkness (with center line) t Total, non-central (without central line) (T) Ring-shaped, central solar eclipse r Ring-shaped, non-central (R) A ring-total rt Partial darkness p

darkness areas

Fig. 3: Area (A): On line 2 , the sun z. Zt. Of the eclipse maximum on (on the central line total, otherwise partial), on line 5 z. Zt. Of the eclipse maximum below.

For all places on line 1 the eclipse begins at sunrise, for places on arc 6 at sunset. On line 3 , the eclipse ends at sunrise, on arc 4 at sunset. This eclipse occurs in middle latitudes and in the equatorial area.

Fig. 4: Area (B): The center line begins and ends in the area of origin or begins and ends in the dungeon area, on the line of the eclipse maximum. This type of eclipse is nowhere visible at noon and occurs in high geogr. Spread up. The lines of the rising and setting area converge in point 5 . There the sun stands at the eclipse maximum exactly in the north or south point of the horizon. Only in the polar area can sunrise and sunset coincide in one place.

Fig. 5 Area (C): The lines intersect at point 5 (polar area), where an observer sees the sun z. Zt. Of the eclipse maximum in the south (missing the northern border in the north) on the horizon.

Fig. 6: Region (D): In this type, the maximum of the eclipse can not be observed anywhere at lunchtime.

Fig. 7 Region (E): partial eclipse. A central line with totality zone is missing. The largest eclipse occurs at point 11 (visible on the horizon). This point is the minimum distance between the moon shadow axis and the center of the earth (gamma).

Fig. 8: Area (F): In this type a small totality area ( 15 ) is created on the line eclipse maximum at sunrise (on the horizon). 0.9972 <gamma <1,026.

Fig. 9: Region (G): This type of eclipse is visible either only in the morning or in the afternoon. An up or down area is missing. The sun is in this area only a little touched by the moon. The largest eclipse occurs in point 11 .

fundamental plane

Here, the cross sections of the moon's core and partial shadows are projected onto a plane perpendicular to the shadow axis and through the center of the earth. It forms the fundamental plane for a rectangular coordinate system (x, y, z) . The x- axis as the intersection of the fundamental plane with the equatorial plane points to the east; the y- axis points north; the z- axis runs parallel to the shadow axis and points to the moon ( Fig. 10). x, y ( 11 = radius of the half-shadow), ( 12 = radius of the core shadow on the fundamental plane) and μ (angle of the shadow axis from Greenwich) are the eclipses ( Fig. 11). From these elements, the darkness conditions for each location of the earth's surface are determined.

Darkness course on the fundamental level

Fig. 12: Area (A): The markings of the lines AB form the northern limit, and the line EF the south limit line of the eclipse area (A) - see Fig. 3. The letters CD limit the length of the central line. Both half and core shadows run over the earth.

Fig. 13: Area (B): The central line cuts the central meridian only out of the earth. The darkness is therefore not visible at noon (see Fig. 4). The center line begins and ends in the ground of the Earth because the centerline CD on the Fundamental plane twice intersects the Sunrise edge of the Earth.

The core shadow cone enters and exits at the sunrise edge. Since the northerly part of the penumbra protrudes far beyond the edge of the earth, the northern boundary line of the eclipse area of FIG. 4 is missing.

Fig. 14: Region (C): The northern part of the moon half shadow extends beyond the edge of the earth, so that the corresponding northern boundary line AB in Fig. 5 is missing. The eclipse is central, however, because the shadow axis CD lies within the Earth orbit (gamma <0.9972).

Fig. 15: Region (D): The northern part of the penumbral cross section AB runs only just below the edge of the earth, so that the northern boundary line AB can only be short ( FIG. 6). The line NB still forms a small sunrise area, so that the line AB is the morning line (Central Meridian: 12 o'clock line).

Fig. 16: Area (E): The core shadow cone of the moon runs outside the edge of the earth (gamma greater than 0.9972), which is still partially within the penumbral area; therefore only a partial solar eclipse is possible (see Fig. 7).

Fig. 17: Area (F): This rare eclipse occurs when the edge of the shadowy shadow touches the top or bottom edge of the earth - which only occurs in high latitudes. Since the core shadow axis does not touch the earth's surface, no central line is formed (see Fig. 8).

Fig. 18: Area (G): The half shadow border CD of the moon touches the top or bottom edge of the earth. The core shadow does not cut the center line NS . The darkness is visible either only in the morning or in the afternoon (see Fig. 9).

Mercury and Venus passages before the sun

Mercury and Venus are inner planets orbiting the sun within Earth's orbit. Under certain conditions, it is therefore possible that these two planets can cross the solar disk. This is the case when a lower conjunction (planet between sun and earth) occurs near a node of the planetary orbit. Mercury passages take place 13 times in the century, while within a period of two and a half centuries, only 4 Venus passages occur. Merkur has a repetition rate of 46 years. Mercury crossings occur at intervals of 13, 7, 9.5, 3.5, 9.5 and 3.5 years ( Figure 10).

Sun and earth globe

Rendering of the eclipses on the earth globe. Time and sight freely selectable. Cities clickable ( Figures 20, 21, 22, 23 and 24).

Date: 11.8.1999 (key <K < Δ T 65 sec.) time: 12 (12 o'clock UT = 13 o'clock CET) Geogr. Width: 48.0818 (48 ° 08'18 '' n. Br.) Geogr. Length: 11.3430 (11 ° 34'30 "'L.) Place name: Munich Height NN: 500 Key <F < Blackboard (K): Select darkness.

Columns 1, 2 and 3: date and time of Sun-Moon conjunction in Right Ascension (AR). From the entered date there are 22 eclipses for optional.

Panel H appears. Line 1 to 5: date, time, latitude and longitude of the beginning and end of darkness. The centrality begins on 11.8.1999 at 9 h 30.3 m UT at 41 ° 2.8 'n. Br and -65 ° 5' westl. Length. Line 3: mid-darkness at noon at 10 h 51.2 m UT at 46 ° 48.3 'n. Br and 18 ° 31.6' ö. L. The eclipse center at midday or midnight true local time forms the center of the globe. Line 6: Minimum distance moon-shadow axis-center of the earth at 11 h 3 m UT (12 h 3 m MEZ) with (gamma) 0.5065 earth radii. If gamma is between 0.968 and 0.9974, it is possible that, despite centrality, there is no northern or southern boundary of the central line, in the case of total or annular eclipses. If gamma is between 0.874 and 0.997, it may happen that there is no central line at midday or midnight, even in otherwise central darkness. If gamma lies between 0.997 and -0.997, then the eclipse is central (earth flattening ignored: gamma = 1. The earth flattening is taken into account at 1 / 298.25). With positive gamma, the eclipse takes place in the northern hemisphere, negative in the southern hemisphere. Line 7 to 11: Date, time and position angle of the local phase sequence. The position angle is here measured from the vertex of the solar disk (vertex) counter-clockwise in a full circle (0 ° .. 360 °).

Line 12 to 14: Date and time of the max. or biggest Eclipse for the place entered (local course), Position angle, duration, coverage percentage, altitude and altitude Azimuth of the sun for this time.

Fig. 25: Sequence of darkness on the sun globe. (Extension level 1). The darkness is totally visible in Munich (100.87%). Duration 2 min. 15 s.

Table I shows the data for the local course of the total darkness in Hamburg, which is only partially visible there, since this location lies north of the central line, but still in the eclipse area. In Hamburg, only a max. Eclamation of 88% can be observed ( Figure 26). For a location on the center line, the sun is totally covered, with only faint stars visible in the vicinity of the sun ( Fig. 27).

Panel J shows the data of a partial solar eclipse. The largest phase (78.7%) of the eclipse occurs at 9 h 37.8 m UT , at 61 ° 26.9 'n. Br and -33 ° 42' westl. Dyn. Length. The local course of this darkness for Frankfurt / M. shows only an eclipse share of 58% at 9 h 47.2 m DT . Column 3 shows that for a partial eclipse, gamma is greater than 0.9972. Fig. 28 shows the max. Phase for Frankfurt / M on the sun globe.
Key <T <

Plate L. Columns 1 to 7: date, time, geogr. Br. And Length of the center line. Column 5: respective solar altitude of until sunset (refraction ignored). Column 6: Duration of totality (negative, total darkness, positive, annular eclipse). Column 7: Width of the totality zone in km.

Panel M. Columns 1 to 6: date and time of geogr. Latitude and longitude of the northern and southern boundary of the central line.  

Panel N: Lines 1 and 2: Ecliptic length and width the sun. Equinox points Spring beginning 0 °, beginning of autumn 180 °, Solstitialpunkte summer beginning 90 ° and beginning of winter 270 ° ekl. L. Counting the right ascension from the vernal equinox. Beginning of spring 0 °, beginning of summer 6 o'clock, autumn beginning 12 o'clock, Winter beginning 18 o'clock.

Declination: Deviation of the Sun or the Moon (line 27) from the equator (therefore corresponds to the latitude after row 9 [sun] and line 31 [moon with consideration of earth flattening]). Deklin. 0 ° = standing on the equator, + 90 = north pole, -90 ° south pole. The sun, however, can deviate only ± 23.5 from the equator, the moon up to ± 28.8 °. Altitude and azimuth (Sun lines 5 and 6) geocentric, Line 21 and 22 topoz. Horizon: height = 0 ° (topoz h -0 ° 50 '= Sun or moon top edge disappears on the horizon), zenith + 90 °, Nadir -90 °. Azimuth: South 0 °, West 90 °, North 180 °, East 270 °, south (0 °) 360 °. Parallax line 7: radius of the Earth seen from the sun. Parallax line 30: radius of the Earth seen from the moon. Line 8: Distance of the sun in astronomical Units (1 AU = 149 597 870 km). Lines 9 and 10: geogr. width and length of the place with the sun in the zenith. Lines 31 and 32: Earth location for which the moon stands in the apex of the sky (moon in the Zenith, height + 90 °). Line 11: Hour angle of the spring point. Time of the respective Rectification Circle in the north-south circle (Sky meridian) of the location (entered geogr. Longitude = north-south line). Is the right ascension of the sun or the moon is equal to the time of the stars, are the stars in the north-south circle of the location whose length was entered. Line 12: Length of the central meridian of the sun. Line 13: Heliogr. Width (elevation of the earth over the solar equator). Lines 12 and 13 indicate for which place on the sun the earth stands in the zenith. Line 14: Position angle of the rotation axis (from north counterclockwise 0 ° .. 360 ° measured). Line 15: Parallactic angle between north and north Zenith direction.  

Line 16: Apparent geoz. Angle radius of the sun. row 17 to 22 like 1 to 6, only on the topoz. Horizon of standing or observation sites (height above apparent Horizon at an eye level of 0 °. Refraction excluded). Line 33: Scheinb. Angular radius of the moon the center of the earth. Line 43: Scheinb. Angle radius of the moon related to the observation site. Line 44: Julian Days from 1.1.4712 BC Chr. Lines 34 and 35: length and Latitude of Earth on the Moon (geocentred), lines 41 and 42: topozentr. Line 36: Length of the light limit. Line 37: survey the sun over the lunar equator. Line 38: Position angle of Moon axis (full circle counterclockwise from earthly North). Line 39: Position angle of the moon phase. Line 40: Parallakt. Angle between north and zenith direction.  

ATTACHMENT

The Christian chronology calculates the calendar years Christ's birth. The one in charge of setting the calendar Monk Dionysius Exiguus (500-556) erred for 5 years. In addition, the number "0" between 1 v. And 1 AD except Eight left. The astronomical-mathematical count is therefore to be distinguished from the historical one.

1900 n. Chr. (Hist.) = 1900 (astronom.)
1 AD (hist.) = 1 (astronom.)
1 v. Chr. (Hist.) = 0 (astronom.)
2 v. Chr. (Hist.) = -1 (astronom.)
4000 BC (Hist.) = -3999 (astronom.)

Historical data v. Are to diminish by 1 and to enter negative.

Date entries from 15.10.1582 refer to the Gregor., Before that on the Julian calendar.

A number of European countries used to the 19th century the Julian calendar. To the rel. in the new style the following differences apply:

1.3.1500-29.2.1700 = 10 days
1.3.1700-29.2.1800 = 11 days
1.3.1800-29.2.1900 = 12 days
1.3.1900-29.2.2000 = 13 days

The input accurate to 0.1 degrees is generally sufficient. For more precise inputs with arc minutes and seconds accuracy serve the following examples:

Geogr. Coordinates of the Cologne Cathedral (Dachreiter): 50 ° 56'33 "north latitude and 6 ° 57'33" east longitude. Input in the form: Geogr. Width: 50.5633. Geogr. Length: 6.5633.

After the number of degrees a separating decimal point (when entering the geogr. Width and length never use commas), behind the Values for arc minutes and arc seconds. Southern geogr. width from Cape Town: -33 ° 58'06 ''. Input: Geogr. Width: -335806.

Southern geogr. Always enter width with a negative sign. Fill in missing places: 56 ° 1'1 '' = 56.0101; 1 ° 1'10 '' = 1.0110; -0 ° 0'1 "= - 0.0001.

The geogr. Length is counted from zero meridian in Greenwich: 180 degrees positive to the east (eg 139 ° 45 ', east longitude Tokyo) and 180 degrees negative to the west (eg -73 ° 58 'west Length New York). The western geogr. Length gets a negative Sign. Always input in sexagesimal form: Degree, Arc minutes and arc seconds (°, ',' ').

Central European Time (CET) is reduced by 1 hour, to obtain world time (in summer time 2 hours). Input example: Time: 17.30095 (18 h 30 m 9.5 s CET). Fill missing positions with zero: 2 h 30 m 1 s = 2.3001.

Button <A <: Input world time, automatic calculation of the Korrektionswerts Δ T 1 minute time (UT = TDT Δ T).

Key <K <: Enter world time and the correction value Δ T according to Tab. P. 24 for calculation to the second (UT = TDT - Δ T) .

Key <D <: Each time entry is terrestrial dynamical time (TDT = DT) , which differs by the difference Δ T from the world time (TDT = UT + Δ T or TDT = TAI + 32.184 sec. TAI = international atomic time) ,

Both the entered and the output length of a place then no longer refers to the geographical zero meridian of Greenwich, but to the dynamic zero meridian, based on the geogr. Length 0.0041781 ° · Δ T ( Δ T in time seconds) east of the geogr. Zero meridians is located.

From dynamic length and time you get geogr. Length and world time using the following correction: UT = TDT - Δ T.

Geogr. Length = east dynamic length + 0.0041781 ° · Δ T.
Geogr. Length = west dynamic length + 0.0041781 · Δ T.

Δ T = TDT-UT

The very precise time determination with quartz and atomic clocks promoted revealed that the earth's rotation is slightly irregular Fluctuations and a slowdown, due to tidal friction, subject.

The course deviation of the Earth's rotation, which over time sums up considerably, was z. B. 1871 -0.005 sec. And 1907 +0.002 sec. These fluctuations probably have their cause in mass displacements in the Earth's interior and meteorological Operations. As a result of tidal friction the earth rotation decreases 0.0016 sec. Over the course of the century.

Time determination from astronomical observations is not very constant; It is therefore assumed that the artificial time (inertial time TDT) is completely uniform and that it is best reproduced today by atomic clocks.

The UT can not be foreseen because the fluctuations are not predictable. The exact correction value Δ T can therefore be determined only from purely astronomical observations of the moon (star coverings, eclipses), or with atomic clocks in comparison with meridian passages of the stars.

The difference ( ΔT ) between UT and the atomic clock-controlled TDT adds up considerably over time and was e.g. B. 1951 years BC +11 hours and 34 minutes

Δ t = 24349 + 72318 T * 29.95 * T ² + (fluctuations): In order to get exactly the correction value Δ T for past and future centuries to one minute, this approximation is valid.

Δ T in century from 1900 (2499-1900) / 100 = T 5.99 = T ² = 35.88.

Δ T in 2499 = 1532 sec. (Input always in sec.).

The respective second-exact correction value Δ T is in the annually appearing astronomer. Yearbooks, z. B. "Calendar for star friends", JA Barth-Verlag, Leipzig.

Claims (1)

The sun globe is characterized by a first-time execution. Lifelike reproduction covers all phenomena, from 1.1.5001 BC. To 31.12.4999 AD, such as solar eclipses, sunspots, prominences, corona, stars and planets near the sun, etc.
The solar globe shows the course of eclipses in REAL TIME, the earth globe, day / night side and twilight zone, the totality zone and the darkness, the fundamental plane the wandering core and partial shadow of the moon.
Rendering of all Mercury and Venus passages for 10 000 years, with entry and exit times, transit time, etc. Additional: graticules, enlargements (telescope) and extension of the sky detail with stars and planets. Information by clicking. All technical and physical data available in tabular form.
The rotatable, three-dimensional precision instrument not only serves the improved observation of the sun and darkness, in addition to its scientific value, the globe, for everyone, interesting and instructive.
The invention is based on the object, all eclipses in the past, present and future, in their lifelike process, over a period of 10,000 years, play.