For 2013, estimated world energy consumption was 5.67 × 1020 joules, or 157,481 TWh. According to the IEA the total world energy consumption in past years was 143,851 TWh in 2008, 133,602 TWh in 2005, 117,687 TWh in 2000, and 102,569 TWh in 1990.

This net flow of energy into and out of the Earth system is Earth’s energy budget. The energy that Earth receives from sunlight is balanced by an equal amount of energy radiating into space. The energy escapes in the form of thermal infrared radiation: like the energy you feel radiating from a heat lamp.

From convective currents (rising air warms the atmosphere). Condensation /Deposition of water vapor (heat is released into the atmosphere by process). At the earth’s surface – Energy absorbed is balanced with the energy released. Absorbed shortwave radiation from the sun.

The Earth’s internal heat source provides the energy for our dynamic planet, supplying it with the driving force for plate-tectonic motion, and for on-going catastrophic events such as earthquakes and volcanic eruptions.

Health impacts and benefits Climate stabilization is important for the safety and security of Earth’s species. Ecosystem protection, management, and carbon sequestration strategies help slow the current rate of changing climate averages and variability, buffering humans from the negative aspects of such change.

Stable: Earth’s climate system is very stable. Global warming will have little or no effects.

gravity

Our planet’s climate is remarkably stable, and has remained in a narrow, liveable, range for almost 4 billion years. The cycle begins with volcanoes spewing CO2 into the atmosphere, which helps keep the planet warm, thanks to the greenhouse effect. This warmth allows seawater to evaporate, forming clouds and rain.

Explanation: Mercury, like the other planets, is in a stable orbit around the Sun. So, Mercury is unlikely to fall into the Sun. In about 6 billion years time, the Sun will run out of Hydrogen fuel in its core.

The sun is currently classified as a “main sequence” star. This means that it is in the most stable part of its life, converting the hydrogen present in its core into helium. Our solar system is just over 4.5 billion years old, so the sun is slightly more than halfway through its stable lifetime.

The sun is growing. And shrinking, and growing again. Every 11 years, the sun’s radius oscillates by up to two kilometres, shrinking when its magnetic activity is high and expanding again as the activity decreases. We already know that the sun is not a static object.

Life has an incredible amount to teach us about living well on planet Earth, in no small part due to the fact that it’s been thriving here for 3.85 billion years. But, how long is that really? If we take the age of Earth—4.5 billion years—and compress it into one year 144 years would be 1 second!

On the biggest steps in early human evolution scientists are in agreement. The first human ancestors appeared between five million and seven million years ago, probably when some apelike creatures in Africa began to walk habitually on two legs.