Sentences with phrase «of photosphere»

Same for the temperature measurements, what part of the photosphere is the correct solar temperature?

The difference between modeled and observed TSI might be the result of underrepresented weak magnetic fields in the Carrington rotation synoptic charts, an uncertainty in the TSI measurement, or a decline of the global temperature of the photosphere.

If a band is free of lines, that cooling capacity is unhindered; but if it has important absorption lines, it will be «blocked» = > the same sort of photosphere questions we have discussed before: a high - altitude photosphere means little power can be transported through that band, whereas an unencumbered band has its photosphere at ground - level.

EGHE, where atmospheric opacity to LWR raises height of topopause, reduces temp of photosphere, causes temperature rise at surface: this seems like a case of the tail wagging the dog; dare I use the term unphysical.

2) As you say, when more GHG is added, the altitude of the photosphere rises (I don't see that the tropopause would rise), and its temperature is reduced: so less power must be radiated away.

You say that where the OD = 1 point, which represents the radius of the photosphere for IR, and as the concentration of CO2 increases, this radius shifts upwards.

That means that CO2 is in a leveraged position (near the top) to influence the altitude of the photosphere.

The Sun's radius is measured from its center to the edge of the photosphere.

During partial eclipses most sunlight is blocked by the Moon passing in front of the Sun, but the uncovered parts of the photosphere have the same surface brightness as during a normal day.

The solar atmosphere is made up of the photosphere, the chromosphere, a transition region, and the corona.

The solar atmosphere above that consists of the photosphere, chromosphere, a transition region and the corona.

Therefore, the outer edge of the photosphere looks dark, an effect called limb darkening that accounts for the clear crisp edge of the sun's surface.

However, the sun's is composed of the photosphere, the chromosphere and the corona.

Data about the magnetic field of the photosphere, which is colder and denser than the corona, were collected by the satellite and enabled the researchers to calculate the evolution of the magnetic environment in the corona during this period of time.

Between 1,500 kilometers from the top of the photosphere and 10,000 kilometers is a region called the «transition zone,» which is where the atoms are accelerated.

Not exact matches

The structures are anchored in the dense photosphere, the visible surface of the Sun.

At its closest it will be within 4 million miles of the roiling solar surface, known as the photosphere.

To unknot the photosphere's tangled mats, the corona must release some of the energy stored there, Caspi says.

Just keeping count of the number of spots, for example, led to recognition of the 11 - year sunspot cycle that waxes from «solar minimum,» when very few spots are seen, to «solar maximum,» when great conglomerations of planet - size splotches pockmark the photosphere, or visible surface of the sun.

The older idea that acoustic waves flowing out of lower levels heats the corona was abandoned in the 1970s, when the Orbiting Solar Observatory 8 spacecraft did not see such waves in the chromosphere, the layer just above the photosphere (the apparent «surface» of the sun in visible light).

«The fact that the outermost region of the sun's atmosphere is at millions of degrees while the temperature of the underlying photosphere is only 6,000 kelvins (degrees C. above absolute zero) is quite nonintuitive.

A sunspot is a region on the Sun's surface (photosphere) that is marked by a lower temperature than its surroundings and intense magnetic activity, which inhibits convection, forming areas of low surface temperature.

Total solar eclipses, seen from Chile on April 16, 1893 (left) and from Mexico on March 7, 1970 (right), reveal the sun's powerful corona, streaming from its photosphere at temperatures of more than 1,000,000 degrees F.

It will do this via high - speed (sub-second timescales) spectroscopic and magnetic measurements of the solar photosphere, chromosphere and corona.

«White - light flares correspond to the most extreme cases of this phenomenon, where so much energy is dumped into the chromosphere and corona that the energy propagates downward to the photosphere, heating it up, and producing the excess brightness that we observe in white light,» according to another of the authors, Jorge Sánchez Almeida, of the Instituto de Astrofísica de Canarias (IAC).

The corona is heated to millions of degrees, yet the lower atmospheric layers like the photosphere — the visible surface of the Sun — are only heated to a few thousand degrees.

This result is in very good agreement with observations carried out on the photosphere and the corona: the formation of the magnetic rope coincides with changes in sunspots in the region of the flare and with the emergence of other structures3.

The Sun's atmosphere is made up of a number of layers including the photosphere, which is the equivalent of the Sun's surface, and the corona, the outermost region where flares take place.

The difference between the assumed lightsource (stellar disk) and the actual lightsource of unknown spectrum (photosphere under the chord) imprints itself onto the transmission spectrum observed.

The mass loading required in this model can be achieved through interaction with the interstellar medium (ISM), the sputtering of the dwarf atmosphere by auroral currents, a volcanically active orbiting planet or magnetic reconnection in the photosphere.

In reality, the stellar spectrum does not cancel out in transmission spectroscopy, because the first - order approximation described above confusingly equates two different light sources: the stellar disk (the spectrum of which is observed before the transit) and the actual light source, which is just a very small fraction of the stellar disk — the projection of the transit chord onto the stellar photosphere (see figure).

Stars are not perfect: in reality, no patch of the stellar photosphere has the same exact spectrum as the stellar chord.

It was long thought that objects at the transition region would display photospheres with patches of clouds and cloud - free regions.

The temperature of a star determines its spectral type, because the energy modifies the physical properties of the plasma in the photosphere.

Because there is a temperature gradient between the core of a star and its surface, energy is steadily transported upward through the intervening layers until it is radiated away at the photosphere.

[17] The star is radiating 1.5 [10] times the Sun's luminosity from its photosphere at an effective temperature of 6,149 K. [11]

To see what sunspots looks like using modern instrumentation, here are two images of the sun's photosphere, taken by the Solar and Heliospheric Observatory (a joint project of NASA and the European Space Agency).

Question from the week before: What is the third most common element in the photosphere of the Sun by weight?

The star's photosphere, or «surface» as seen in visible light, varies in size as it pulsates from about the diameter of Mars» orbit around the Sun to that of the asteroid belt.

The outer atmosphere will expand significantly, and planet Earth will lie within the Sun's photosphere (the part of the Sun that is not transparent to light).

To carry out novel investigations based on spectro - polarimetric observations with ground - based and space solar telescopes, with emphasis on the study of the magnetic field in chromospheric and coronal structures and its coupling with the underlying photosphere.

The corona can be seen only during solar eclipses because it is millions of times fainter than the photosphere.

The part of the Sun that we see from Earth is called the photosphere.

The photosphere is the lowest layer of the sun's atmosphere, and emits the light we see.

Since the outer gas envelopes of the stars are in contact (overflowing their Roche lobes), they essentially share a common photosphere despite having two distinct nuclear - burning cores.

The photosphere is the lowest region of the sun's atmosphere and is the region that we can see.

High - dispersion spectroscopy confirmed the presence of light from a cool stellar photosphere in the spectrum of this system.

It extends millions of kilometers into space and is a million times fainter than the photosphere.

«The surface of the sun» typically refers to the photosphere, at least in lay terms.

As gases churn in the photosphere, they produce shock waves that heat the surrounding gas and send it piercing through the chromosphere in millions of tiny spikes of hot gas called spicules.