OMC-2 FIR 4
Credit: Herschel image: ESA/Herschel/Ph. André, D.
Polychroni, A. Roy, V. Könyves, N. Schneider for the Gould Belt survey
Key Programme; inset and layout: ESA/ATG medialab.
Results from Herschel may have helped to solve a puzzle
surrounding our own Sun's past. By studying very young stars in the
Orion Nebula, astronomers have been able to gain an insight into how the
Sun may have been behaving in its youth.
By using the HIFI spectrometer to detect the far-infrared light at
very specific frequencies, the team obtained the chemical fingerprint of
a range of atoms and molecules within the clump of gas and dust in
which the stars are forming. This also allows a study of the
temperature, and showed that the gas and dust are relatively warm,
though still at around -200 Celsius. It is thought that the Sun formed
in a similar environment, and so studies of such regions allow
astronomers to examine one possible history of the Sun's life.
The mystery about our own Sun relates to evidence for a particular
form, or isotope, of the element beryllium in meteorites found on Earth.
This particular isotope, called beryllium-10, is relatively unusual in
that it is not formed in the fusion reactions within stars, or in the
supernova explosions which occur when massive stars die. Rather, it is
formed when very energetic particles slam into heavier, and more common,
elements such as oxygen.
Beryllium-10 doesn't normally hang around, though, because it decays
into a specific set of lighter elements. The fact that breyllium-10 is
present means that it was being created as the rocks formed, which
suggests the that material in the early Solar System was being bombarded
by very energetic particles. The big question has been whether these
particles were produced by the young Sun, or whether they originated
further afield in the deaths of massive stars.
One way of gaining a handle on that question is to study stars at a
similar stage of their life - hence the interest in the young stars in
Orion. An interesting result from the latest study was the relative
amounts of molecules containing hydrogen combined with other atoms such
as carbon, oxygen and nitrogen. In most star-forming environments the
nitrogen-bearing molecules such as diazenylium (N2H+) are destroyed relatively easily, leaving an over-abundance of molecules such as hydrogen carbonate (HCO).
However, in the case of this particular clump, known as "OMC-2 FIR4",
it appears that the HCO has been destroyed almost as quickly as the
N2H+. The only explanation for the destruction of both types of molecule
is a surprisingly high rate of energetic particles - and at a rate
easily high enough to explain the presence of beryllium-10 in the
meteorites. While it doesn't rule out other possibilities, it is strong
evidence that the Sun may have been much more active in its youth.
