ESA Science & Technology - SOHO's latest surprise: gas near the Sun heading the wrong way

About 8000 inflow events have now been logged - most of them since 1998 while the Sun has been at its most active, as judged by the high count of sunspots. The inflows can start at an altitude of up to 2 700 000 kilometres above the visible surface, a distance equal to twice the Sun's diameter. Here the accelerating solar wind, leaving the Sun, has reached a speed of about 120 kilometres per second. Fighting against it, the gas clouds travel in at 50-100 kilometres per second. Typically they appear to come to rest about 700 000 kilometres out.

"I was stunned when I saw the first movies showing these inflows," says Bernhard Fleck, ESA's project scientist for the space mission. "Before this discovery by SOHO no one had any idea that gas could travel the wrong way, and be pushed back towards the Sun. Now we must learn from the inflows how the Sun regulates the magnetic fields carried by the solar wind, which are a key driver for the space weather we experience in the Earth's vicinity."

The LASCO instrument blots out the intense direct light from the visible surface, to keep the Sun permanently in eclipse. A multinational scientific team that includes the United States Naval Research Laboratory, France's Laboratoire d'Astronomie Spatiale, Germany's Max Planck-Institut f|r Aeronomie, and the United Kingdom's Birmingham University, contributed LASCO to SOHO. LASCO is already famous for registering explosive mass ejections from the Sun, and discovering many sungrazing comets.

Even with this powerful instrument, the inflows are hard to see. Most useful for the purpose is the LASCO C2 component, which shows the region from 700 000 to 3 500 000 kilometres from the visible surface. At the Naval Research Laboratory, Neil Sheeley and Yi-Ming Wang find the inflows by subtracting one electronic image from the next, taken 20-25 minutes later, and assembling a series of such difference images into a movie. The human eye is then good at spotting unusual, inward movement against the general background of outflowing gas.

Although the gas feels a very strong pull from the Sun's gravity, this is not the decisive force acting on the inflows. The high rate at which they gather speed initially, and their eventual slowdown, suggest instead that they are firmly under the control of a magnetic force. A few inflows are a backwash from explosive mass ejections, which are sporadic events, but the overwhelming majority occur quite regularly within regions of slow solar wind.

A downpour of 20 inflows per day, seen on the left side of the Sun, can be followed after a lull of two weeks by a similar downpour seen on the right side. This means that the occurrences persist in a particular region on the Sun, which takes two weeks to move from left to right as the Sun rotates. The regional association can continue for months, and suggests to Sheeley and Wang how the inflow regions and the magnetic field are related.

Near the Sun's surface the magnetic field is a patchwork, with field lines looping outwards from some places and back in at others. The solar wind drags the longest loops far out into space, creating contrasting sectors where the magnetic field lines are directed in opposite senses. Before the solar wind has reached its full speed, opposing field lines can short-circuit at a boundary between sectors, to form new magnetic loops. These collapse towards the Sun, carrying with them the inflowing gas clouds now observed.

"We are seeing something opposite to what we expected," says Sheeley. "Normally, when this happens, we initially doubt the observation - suspecting, for example, that the movie is running backwards. But when we confirm that the observation is really correct, we are forced to change our way of thinking. Such mind-changing discoveries help us past temporary snags in our understanding and inevitably lead to progress."

In this case, one area of progress may concern magnetic fields and their effects on Earth. If Sheeley and Wang are right in thinking that the inflows indicate collapsing magnetic loops, pulling material inwards against the outward drag of the solar wind, then these are showing us how the Sun recycles the magnetic field in its atmosphere. This recycling process regulates the strength of the interplanetary magnetic field that extends outward past Earth and affects space weather.

SOHO's inflows thus provide unexpected clues to what influences solar magnetic activity near the Earth and all across the Solar System. Apart from magnetic storms, which can harm technical systems, there is growing interest in the shield that the interplanetary magnetic field provides against cosmic rays. These energetic particles from the Galaxy can cause genetic mutations in living things and glitches in computers, and some scientists think they are also involved in cloud formation on the Earth. But their variations have puzzling features.

Reductions and increases in cosmic rays reaching the Earth are not in perfect step with rising and falling sunspot activity. And when sunspot cycles were of longer duration, 100 years ago, the interplanetary magnetic field was weaker and the cosmic-ray intensity was on average higher than nowadays. The 'mind-changing' discovery of the inflows near the Sun may lead to better explanations of these variations, and eventually to predictions of cosmic-ray intensities.

SOHO is a project of international cooperation between ESA and NASA. The spacecraft was built in Europe for ESA and equipped with instruments by teams of scientists in Europe and the USA. NASA launched SOHO in December 1995, and in 1998 ESA and NASA decided to extend its highly successful operations until 2003.

For more information please contact:

Dr. Bernhard Fleck
ESA-SOHO project scientist
ESA Space Science Dept
c/o NASA-GSFC, Greenbelt (Maryland USA)
Tel: +1 301 286 4098
Fax: +1 301 286 0264
Email: bfleckesa.nascom.nasa.gov