Sentences with phrase «radiation pressure from»

Ok, don't see where you gave where any of the numbers are coming from but it suffices you seem sure the radiation pressure from added GHG molecules (H2O or CO2), let's say 10 per million is so infinitesimally small that the lift of the atmosphere in every cubic meter per one meter layer up to say 80 km is so insignificant it can be totally ignored.

Ehrenreich and his team think that such a huge cloud of gas can exist around this planet because the cloud is not rapidly heated and swept away by the radiation pressure from the relatively cool red dwarf star.

Now, Hippke and Heller show that a combination of the stars» gravity and radiation pressure from their photons can bring the craft into a stable orbit around one of the stars, then around the tantalising planet (Astrophysical Journal Letters, doi.org/bx8t).

Atoms are slowed and cooled by radiation pressure from laser light and then trapped in a bottle whose walls are magnetic fields.

Incrementally adjusting its angle as it approaches to soak up more radiation pressure from the stars, that sail could bleed off enough speed to be captured into orbit within the system.

Not exact matches

When pressure is higher, it better shields the surface from radiation.

The X-ray data also indicates that radiation from material surrounding this black hole has consistently surpassed the so - called Eddington limit, defined by a balance between the outward pressure of radiation from the hot gas and the inward pull of the gravity of the black hole.

Vinković's model «shows how dust grains propelled by radiation pressure can travel from the disk's hottest regions to its icy outer edges,» says astronomer Dániel Apai of the Space Telescope Science Institute in Baltimore, Maryland.

Results from recent clinical trials and studies in animals suggest that a class of anti-cancer drugs called angiogenesis inhibitors may be able to temporarily reduce interstitial pressure and improve the efficacy of chemotherapy and radiation treatments.

Plants were grown either with natural solar radiation only (the control), natural solar radiation plus supplemental lighting from high - pressure sodium lamps, or natural solar radiation plus supplemental light from intracanopy (IC) LED towers.

New work from Carnegie scientists using intense infrared radiation shines new light on this fundamental material at extreme pressures and reveals the details of a surprising new form of solid hydrogen.

But as astronomers report online today in Nature, the galaxy is losing more gas than this — between three and 30 solar masses per year — as winds, radiation pressure, and supernova explosions from the starburst itself drive gas away.

This radiation pressure propels solar sails and helps direct comet tails so they always point away from the Sun.

The smaller debris / meteoroids produced get spread around the orbit quite quickly (read: centuries or millennia) by various physical effects (ejection speeds from the comet; radiation pressure; Poynting - Robertson effect; Yarkovsky effect).

These might arise from mechanical effects — for example, selective radiation pressure or photospheric diffusion and element separation — rather than from nuclear effects.

Good arguments exist that the central regions should collapse first, producing a condensed protostar whose contraction is halted by the large buildup of thermal pressure when radiation can no longer escape from the interior to keep the (now opaque) body relatively cool.

The Sun's radiation pressure and solar wind accelerate materials away from the comet's head at differing velocities according to the size and mass of the materials.

«Once a protostar reaches a threshold of about 20 solar masses, the pressure exerted by its radiation should overpower gravity and prevent it from growing any bigger.

Is star formation triggered mainly by shockwaves from exploding stars, or the pressure created by radiation and stellar winds from massive stars — or can those processes get in the way of the collapse?

In 2010, model simulations of rocky super-Earths between two and 10 Earth - masses indicated that high pressures could keep their cores solid instead of molten, which would prevent a protective magnetic field from forming protecting developing surface life from stellar radiation.

When sunlight from the Sun hits these solar panels, the photons exert a small but significant amount of force (radiation pressure).

However, only on Earth can they stand without special protection from inhospitable temperatures, atmospheric gases and pressure (or its absence), or Solar and cosmic radiation.

Chlorella has been shown to help support healthy hormonal function and good cardiovascular health, fight against the effects of chemotherapy and radiation, help lower blood pressure and bad cholesterol, and excel in removing harmful toxins from your body.

According to the National Cancer Institute, radiation therapy helps shrink tumors so the pressure and the pain resulting from that pressure are relieved in the patient.

For example simple spectroscopy dictates that the CO2 molecule vibrates, stretches, and rotates creating quantized absorption lines that are Doppler broadened and pressure broadened and absorb the infrared radiation coming from the warmed planet.

The basic ingredients are easy to list: — absorption / emission properties (or spectroscopic parameters) of CO2 at atmospheric pressures, i.e. data presently available from HITRAN - database combined with models of line broadening — observed properties of the atmosphere where most important features include clouds and moisture content, but many other factors have some influence — computer model of the transmission of radiation along the lines of MODTRAN or GENLN2

The advantages are said to be: 1) the pressure drop caused by the mesh spreads the airflow evenly over the full surface of the absorber, and 2) the first layer of mesh acts as a radiation shield to reduce the radiation from the hotter inner layers toward the glazing.

Since the LW radiation from the ground is always in the azimuth hemisphere's direction and 1/2 of the reemitted photons are in the nadir hemisphere, a radiation pressure exists here which will cause and infinitesimal but real expansion of the atmosphere which will exactly cause a temperature decrease that exactly counteracts any warming from the downward radiation.

I will keep bring this up every month or two until 1) someone says they clearly see what I am talking about or 2) someone clearly explains how this radiation pressure created by these LW radiations, up from the ground, 1/2 down from GHGs does not cause a pressure which will expand the atmosphere and by thermodynamics fundamental equations will cool the atmosphere in exactly an equal amount.

Was it taking the 390 W / m2 of back radiation in common energy balance charts and calculating from that the upward pressure and therefore the volume expansion?

The greater the atmospheric pressure, the more N2 molecules, the greater the likely - hood that conduction will take place limiting radiation from the surface to space, the more surface temperatures must rise.

If there's no radiation from the Sun, no heat capacity in the model planet, no mass big enough to effect pressure changes («real» ideal gases which don't have mass), nothing much is happening because there's no movement, (movement from the play of hot and cold volumes as hot gases rise and cold sink, becoming less dense and gaining density), but,

While Earth's lower atmosphere is about one percent water vapor (although it seems much higher in the humid Louisiana summers), the upper atmosphere, where ultraviolet radiation can penetrate, is very dry: a cold trap, a combination of pressure and temperature, prevents water vapor from rising high in the earth's atmosphere.

The altitude where the radiation to the cosmos takes place with the associated cooling of the top of the air is near t = 1 from the top of the air, that is at a pressure (1 / tmax H2O)(1/4.5) or (1 / tmax CO2)(1/1.45); the line by line computation of figure 6 - C is a morphing from figure 6 - A.

Temperature is proportional to pressure, therefor Earth atmospheric temperature is formed by background radiation pressure, and distance from the shielding effect of the Sun

The water vapor pressure is below the saturation value of 101325 Pa at 373.15 K (that isn't quite right either, but close enough) so there will be net evaporation of water from the surface as it warms from absorption of radiation and conduction from the water vapor.

Since the water vapor pressure equals the saturation vapor pressure, there is no net evaporation or condensation so there is no flow of energy from the top wall to the water and water vapor or vice versa by radiation or conduction nor to or from the water vapor to the water and the temperature of all components will not change with time.

The simpler approach to calculating the downward radiation from a given gas by the total concentration across say 10 km of atmosphere is going to give a very approximate answer — this is because the absorption lines change their width with pressure and temperature.

He accurately reported that about 10 % of the radiation from a 100 °C black body was absorbed in his tube, and that at lower pressure at most 9.6 % was absorbed, whereas in fact it must have been about 9 %.

Conclusion, CO2 (and its «back radiation») makes LITTLE difference, because at the same level of pressure on BOTH planets, the only thing that seems to matter is planetary distance from the sun.

He then calculates natural sky radiation for varying Terrestrial conditions, varying from the Antarctic plateau (high elevation, low temperature, humidity and pressure) to the tropics (high humidity).

A similar comparison between other planets in the solar system reveals similar relationships between the planets» various distances from the Sun and the planets» various atmospheric pressures, regardless of chemical compositions of the planets» atmospheric gases,... regardless of those atmospheric gases» abilities to produce «back radiation».

Statistics and observations are available from a variety of variables or phenomena such as temperature (2 meter or ground temperature), humidity, wind, air pressure, radiation, cloudiness, visibility, precipitation, snow depth, lightning etc..

We use the 9 climate variables of surface air temperature (SAT), sea level pressure (SLP), precipitation (rain), the top of atmosphere (TOA) shortwave (SW) and longwave (LW) full - sky radiation, clear - sky radiation (CLR, radiative flux where clouds do not exists), and cloud radiative forcing (CRF, radiative effect by clouds diagnosed from the difference between full - sky and clear - sky radiation, Cess et al. 1990).