The spinning magnet of Sun-like stars:
are close-in giant planets forcing the engine?
Stars like the Sun host a spinning engine - their magnetic fields.
These magnetic fields are similar to those of bar magnets, except that they
flip their north and south sides regularly, every 11 years in the case of the Sun.
For the first time, an international team of astrophysicists1 has just
caught one star other than the Sun - tau Bootis A - in the process of
flipping its north and south magnetic poles.
They however suspect that this event is much more frequent in tau Bootis
A than in the Sun - is the magnetic engine in tau Bootis A spun up by the
giant planet closely orbiting its host star?
in the Monthly Notices of the Royal Astronomical Society, should help
scientists understand better how magnetic engines work in stars like our Sun.
Stars like the Sun are not quiet and steady - they host a complex engine
very similar to that of a bar magnet.
The solar corona, best visible during
magnetic field just as iron filings would do for a bar magnet.
The engine producing
magnets of Sun-like stars
is called a
and uses both
the spinning of stars and the boiling-like motions occuring
below their surfaces. The
is also generated by a dynamo engine.
An interesting and important property of the Sun's magnet is its ability to
flip its north and south sides regularly, every 11 years:
this is the
of the Sun, whose impact on the Earth climate is potentially strong
enough to have caused the
little ice age
in the seventeen century. The Earth's magnet is also flipping side, though
much less frequently and more eratically.
Sun-like stars also host magnetic fields and their magnets are
likely flipping side regularly as well;
however, observing such events was difficult until now, as they could only
be detected through indirect tracers, like for instance the very subtle
brightness changes occuring at very specific colors.
By looking directly at the magnetic fields of stars other than the Sun,
an international team of astrophysicists1, led by JF Donati
and C Moutou from CNRS (Toulouse and Marseille),
has recently caught one star, called tau Bootis A, in the process of
flipping its magnet, using twin instruments called
ESPaDOnS2 on the
Telescope3 (atop MaunaKea in Hawaii) and
NARVAL4 on the
pic du Midi
en France). The
they reconstruct for tau Bootis A are also fairly complex.
Slightly hotter and 20% more massive than the Sun,
tau Bootis A
is fairly bright and visible with the naked eye, being located only 51
light years away from us. What makes tau Bootis A even more interesting
is that it harbours a giant planet orbiting very close to the surface of the star.
The planet is actually so close to its host star
and so massive - about 6.5 times more massive than Jupiter and orbiting at
an altitude of only one twentieth the distance between the Sun and the Earth
- that astronomers think it succeeded at forcing at least the surface
of tau Bootis A to corotate with the planet orbital motion through
tidal torques (the
very effect that forced the Moon to corotate with its orbital motion around
If JF Donati, C Moutou and collaborators managed to catch tau Bootis A in this state
of magnetic flipping, it is probably not just by chance. They suspect that
this event is much more frequent in tau Bootis A than in the Sun -
possibly every few years only as opposed to 11 years in the case of the Sun.
Is the giant planet that already managed to speed up the surface of
tau Bootis A, also spinning up the magnetic engine of its host star?
Donati, Moutou and collaborators will undoubtedly keep their eyes tightly focussed
on tau Bootis A in coming years to make sure not to miss any
of the star's future regular magnetic turnover - with the hope of understanding better
how magnetic engines work in stars like our Sun, and whether/how close-in giant
planets manage to spin them up.
Press contacts in UK, USA/Hawaii & Canada:
in UK: Andrew Collier Cameron, University of StAndrews, Tel: +44-1334-463147, email: Andrew.Cameron[AT]st-and.ac.uk
in USA/Hawaii: Evgenya Shkolnik, University of Hawaii, Tel: 808-292-9088, email: shkolnik[AT]ifA.hawaii.edu
in Canada: David Bohlender, National Research Council Canada / Conseil national de recherches Canada, Tel: 250-363-0025, email: david.bohlender[AT]nrc-cnrc.gc.ca
This team includes
JF Donati (Observatoire Midi-Pyrenees/LATT, CNRS/UPS, France),
C Moutou (Observatoire Marseille-Provence/LAM, CNRS/UMP, France),
R Farès (Observatoire Midi-Pyrenees/LATT, CNRS/UPS, France),
D. Bohlender (National Research Council of Canada, Canada),
M Deleuil (Observatoire Marseille-Provence/LAM, CNRS/UMP, France),
C Catala (Observatoire Paris-Meudon/LESIA, CNRS/UP7, France),
E Shkolnik (University of Hawaii, USA),
A.C. Cameron (University of StAndrews, UK),
M.M. Jardine (University of StAndrews, UK) and
G.A.H. Walker (University of Victoria, Canada)
ESPaDOnS was cofunded by France (CNRS/INSU, Ministère de la Recherche, LATT, Observatoire
Midi-Pyrénées, Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire
de Paris-Meudon), Canada (NSERC), CFHT and ESA (ESTEC/RSSD). First light occured on
2004 Sept 2.
CFHT operation is funded by Canada (NRC/CNRC), France (CNRS/INSU) and the University of Hawaii.
NARVAL was cofunded by the Région Midi-Pyrénées, the Ministère de la Recherche, the conseil
Général des Hautes Pyrénées, the European Union (FEDER funds) and CNRS/INSU. First light
occured on 2006 Nov 13.
The Télescope Bernard Lyot (TBL) is funded by CNRS/INSU.