Beta Pictoris
Beta Pictoris (abbreviated β Pictoris or β Pic) is
the second brightest star in the constellation Pictor.
It is located 63.4 light-years (19.4 pc) from the Solar
System, and is 1.75 times as massive and 8.7 times as
luminous as the Sun. The Beta Pictoris system is very
young, only 20 to 26 million years old,[12] although it
is already in the main sequence stage of its
evolution.[8] Beta Pictoris is the title member of the
Beta Pictoris moving group, an association of young
stars which share the same motion through space
and have the same age.[13]
The European Southern Observatory (ESO) has
confirmed the presence of two planets, Beta Pictoris
b,[14] and Beta Pictoris c,[15] through the use of direct
imagery. Both planets are orbiting in the plane of the
debris disk surrounding the star. Beta Pictoris c is
currently the closest extrasolar planet to its star ever
photographed: the observed separation is roughly the
same as the distance between the asteroid belt and
the Sun.[15]
β Pictoris
Location of β Pictoris (circled)
Observation data
Epoch J2000
Equinox J2000
Constellation
Pictor
Right ascension
05h 47m 17.1s[1]
Beta Pictoris shows an excess of infrared emission[16]
compared to normal stars of its type, which is caused
by large quantities of dust and gas (including carbon
monoxide)[17][18] near the star. Detailed observations
reveal a large disk of dust and gas orbiting the star,
which was the first debris disk to be imaged around
another star.[19] In addition to the presence of several
planetesimal belts[20] and cometary activity,[21] there
are indications that planets have formed within this
disk and that the processes of planet formation may
be ongoing.[22] Material from the Beta Pictoris debris
disk is thought to be the dominant source of
interstellar meteoroids in the Solar System.[23]
Declination
−51° 03′ 59″[1]
Apparent magnitude (V)
3.861[1]
Characteristics
Spectral type
A6V[2]
U−B color index
0.10[3]
B−V color index
0.17[3]
Variable type
Delta Scuti variable[4]
Astrometry
Radial velocity (Rv)
+20.0 ± 0.7[5] km/s
Proper motion (μ)
RA: +4.65[6] mas/yr
Dec.: +83.10[6] mas/yr
Location and visibility
Parallax (π)
51.44 ± 0.12 mas[6]
Distance
Beta Pictoris is a star in the southern constellation of
Pictor, the Easel, and is located to the west of the
bright star Canopus.[24] It traditionally marked the
sounding line of the ship Argo Navis, before the
63.4 ± 0.1 ly
(19.44 ± 0.05 pc)
Absolute magnitude (MV) 2.402[7]
Details
constellation was split.[25] The star has an apparent
visual magnitude of 3.861,[1] so is visible to the naked
eye under good conditions, though light pollution
may result in stars dimmer than magnitude 3 being
too dim to see. It is the second brightest in its
constellation, exceeded only by Alpha Pictoris, which
has an apparent magnitude of 3.30.[26]
Mass
1.75[8] M☉
Radius
1.8[9] R☉
Luminosity (bolometric)
8.7[8] L☉
Surface gravity (log g)
4.15[2] cgs
Temperature
8,052[2] K
Metallicity
+0.14[10]
The distance to Beta Pictoris and many other stars
was measured by the Hipparcos satellite. This was
done by measuring its trigonometric parallax: the
slight displacement in its position observed as the
Earth moves around the Sun. Beta Pictoris was found
to exhibit a parallax of 51.87 milliarcseconds,[27] a
value which was later revised to 51.44
milliarcseconds when the data was reanalyzed taking
systematic errors more carefully into account.[6] The
distance to Beta Pictoris is therefore 63.4 light years,
with an uncertainty of 0.1 light years.[28][note 1]
Rotational velocity
(v sin i)
130[11] km/s
Age
23 ± 3[12] Myr
Other designations
GJ 219, HR 2020, CD −51°1620, HD
39060, GCTP 1339.00, SAO 234134,
HIP 27321
Database references
SIMBAD
The Hipparcos satellite also measured the proper
motion of Beta Pictoris: it is traveling eastwards at a
rate of 4.65 milliarcseconds per year, and northwards ARICNS
at a rate of 83.10 milliarcseconds per year.[6]
Measurements of the Doppler shift of the star's
spectrum reveals it is moving away from Earth at a
rate of 20 km/s.[5] Several other stars share the same
motion through space as Beta Pictoris and likely
formed from the same gas cloud at roughly the same
time: these comprise the Beta Pictoris moving group.[13]
data (https://simbad.c
ds.unistra.fr/simbad/si
m-id?Ident=bet+Pic)
data (https://wwwadd.
zah.uni-heidelberg.d
e/datenbanken/aricns/
cnspages/4c00467.ht
m)
Physical properties
Spectrum, luminosity and variability
This video sequence is based on an
artist's impression of exocomets
orbiting the star Beta Pictoris.
According to measurements made as part of the Nearby Stars
Project, Beta Pictoris has a spectral type of A6V[2] and has an
effective temperature of 8,052 K (7,779 °C; 14,034 °F),[2] which is
hotter than the Sun's 5,778 K (5,505 °C; 9,941 °F).[29] Analysis of the spectrum reveals that the star
contains a slightly higher ratio of heavy elements, which are termed metals in astronomy, to hydrogen
than the Sun. This value is expressed as the quantity [M/H], the base-10 logarithm of the ratio of the
star's metal fraction to that of the Sun. In the case of Beta Pictoris, the value of [M/H] is 0.05,[2]
which means that the star's metal fraction is 12% greater than that of the Sun.[note 3]
Analysis of the spectrum can also reveal the surface gravity of the star. This is usually expressed as log
g, the base-10 logarithm of the gravitational acceleration given in CGS units, in this case, cm/s². Beta
Pictoris has log g=4.15,[2] implying a surface gravity of 140 m/s², which is about half of the
gravitational acceleration at the surface of the Sun (274 m/s²).[29]
As an A-type main sequence star, Beta Pictoris is more luminous
than the Sun: combining the apparent magnitude of 3.861 with the
distance of 19.44 parsecs gives an absolute magnitude of 2.4,[7] as
compared to the Sun, which has an absolute magnitude of
4.83.[29] This corresponds to a visual luminosity 9.2 times greater
than that of the Sun.[note 4] When the entire spectrum of radiation
from Beta Pictoris and the Sun is taken into account, Beta Pictoris
is found to be 8.7 times more luminous than the Sun.[8][30]
Artist's impression of the planet Beta
Pictoris b[note 2]
Many main sequence stars of spectral type A fall into a region of
the Hertzsprung–Russell diagram called the instability strip,
which is occupied by pulsating variable stars. In 2003,
photometric monitoring of the star revealed variations in brightness of around 1–2 millimagnitudes
on frequencies between about 30 and 40 minutes.[4] Radial velocity studies of Beta Pictoris also reveal
variability: there are pulsations at two frequencies, one at 30.4 minutes and one at 36.9 minutes.[31]
As a result, the star is classified as a Delta Scuti variable.
Mass, radius and rotation
The mass of Beta Pictoris has been determined by using models of stellar evolution and fitting them to
the star's observed properties. This method yields a stellar mass between 1.7 and 1.8 solar masses.[8]
The star's angular diameter has been measured using interferometry with the Very Large Telescope
and was found to be 0.84 milliarcseconds.[9] Combining this value with the distance of 63.4 light
years gives a radius 1.8 times that of the Sun.[note 5]
The rotational velocity of Beta Pictoris has been measured to be at least 130 km/s.[11] Since this value
is derived by measuring radial velocities, this is a lower limit on the true rotational velocity: the
quantity measured is actually v sin(i), where i represents the inclination of the star's axis of rotation to
the line-of-sight. If it is assumed that Beta Pictoris is viewed from Earth in its equatorial plane, a
reasonable assumption since the circumstellar disk is seen edge-on, the rotation period can be
calculated as approximately 16 hours, which is significantly shorter than that of the Sun (609.12
hours[29]).[note 6]
Age and formation
The presence of significant amounts of dust around the star[32]
implies a young age of the system and led to debate about whether
it had joined the main sequence or was still a pre–main sequence
star[33] However, when the star's distance was measured by
Hipparcos it was revealed that Beta Pictoris was located further
away than previously thought and hence was more luminous than
originally believed. Once the Hipparcos results were taken into
Artist's impression of Beta
account, it was found that Beta Pictoris was located close to the
Pictoris[note 7]
zero age main sequence and was not a pre–main sequence star
after all.[8] Analysis of Beta Pictoris and other stars within the
Beta Pictoris moving group suggested that they are around 12 million years old.[13] However more
recent studies indicate that the age is roughly double this at 20 to 26 million years old.[34][12]
Beta Pictoris may have been formed near the Scorpius–Centaurus association.[35] The collapse of the
gas cloud which resulted in the formation of Beta Pictoris may have been triggered by the shock wave
from a supernova explosion: the star which went supernova may have been a former companion of
HD 83058, which is now a runaway star. Tracing the path of HIP 46950 backwards suggests that it
would have been in the vicinity of the Scorpius–Centaurus association about 13 million years ago.[35]
However, HD 83058 has been found to be a spectroscopic binary and unlikely to have been ejected by
the supernova explosion of a close companion, so the simple explanation for the origin of the Beta
Pictoris cluster is in doubt.[36]
Circumstellar environment
Debris disks
Erika Nesvold and Marc Kuchner
discuss their supercomputer
simulation of how the Beta Pictoris b
planet sculpts the Beta Pictoris
debris disk into a warped spiral
shape.
Hubble Space Telescope image of the main and
secondary debris disks
Excess infrared radiation from Beta Pictoris was
detected by the IRAS[37] spacecraft in 1983.[32] Along
with Vega, Fomalhaut and Epsilon Eridani, it was one of the first four stars from which such an excess
was detected: these stars are called "Vega-like" after the first such star discovered. Since A-type stars
like Beta Pictoris tend to radiate most of their energy at the blue end of the spectrum,[note 8] this
implied the presence of cool matter in orbit around the star, which would radiate at infrared
wavelengths and produce the excess.[32] This hypothesis was verified in 1984 when Beta Pictoris
became the first star to have its circumstellar disk imaged optically.[19] The IRAS data are (at the
micron wavelengths): [12]=2.68, [25]=0.05, [60]=−2.74 and [100]=−3.41. The colour excesses are:
E12=0.69, E25=3.35, E60=6.17 and E100=6.90.[16]
The debris disk around Beta Pictoris is seen edge-on by observers on Earth, and is orientated in a
northeast-southwest direction. The disk is asymmetric: in the northeast direction it has been observed
out to 1835 astronomical units from the star, while the southwest direction the extent is 1450 AU.[38]
The disk is rotating: the part to the northeast of the star is moving away from Earth, while the part to
the southwest of the disc is moving towards Earth.[39]
Several elliptical rings of material have been observed in the outer regions of the debris disk between
500 and 800 AU: these may have formed as a result of the system being disrupted by a passing
star.[40] Astrometric data from the Hipparcos mission reveal that the red giant star Beta Columbae
passed within 2 light years of Beta Pictoris about 110,000 years ago, but a larger perturbation would
have been caused by Zeta Doradus, which passed at a distance of 3 light years about 350,000 years
ago.[41] However computer simulations favor a lower encounter velocity than either of these two
candidates, which suggest that the star responsible for the rings may have been a companion star of
Beta Pictoris on an unstable orbit. The simulations suggest a perturbing star with a mass of 0.5 solar
masses is likely to blame for the structures. Such a star would be a red dwarf of spectral type
M0V.[38][42]
Various planet formation processes, including exocomets and
other planetesimals, around Beta Pictoris, a very young type A V
star (NASA artist's conception)
In 2006, imaging of the system with the
Hubble Space Telescope's Advanced
Camera for Surveys revealed the
presence of a secondary dust disk
inclined at an angle of about 5° to the
main disk and extending at least 130 AU
from the star.[43] The secondary disk is
asymmetrical: the southwest extension is
more curved and less inclined than the
northeast. The imaging was not good
enough to distinguish between the main
and secondary disks within 80 AU of
Beta Pictoris, however the northeast
extension of the dust disk is predicted to
intersect with the main disk at about 30
AU from the star.[43] The secondary disk
may be produced by a massive planet in
an inclined orbit removing matter from
the primary disk and causing it to move
in an orbit aligned with the planet.[44]
Studies made with the NASA Far Ultraviolet Spectroscopic Explorer have discovered that the disk
around Beta Pictoris contains an extreme overabundance of carbon-rich gas.[45] This helps stabilize
the disk against radiation pressure which would otherwise blow the material away into interstellar
space.[45] Currently, there are two suggested explanations for the origin of the carbon overabundance.
Beta Pictoris might be in the process of forming exotic carbon-rich planets, in contrast to the
terrestrial planets in the Solar System, which are rich in oxygen instead of carbon.[46] Alternatively it
may be passing through an unknown phase that might also have occurred early in the development of
the Solar System: in the Solar System there are carbon-rich meteorites known as enstatite chondrites,
which may have formed in a carbon-rich environment. It has also been proposed that Jupiter may
have formed around a carbon-rich core.[46]
In 2011 the disk around Beta Pictoris became the first other planetary system to be photographed by
an amateur astronomer. Rolf Olsen of New Zealand captured the disk with a 10-inch Newtonian
reflector and a modified webcam.[47]
Planetesimal belts
In 2003, imaging of the inner region of the Beta Pictoris system with the Keck II telescope revealed
the presence of several features which are interpreted as being belts or rings of material. Belts at
approximately 14, 28, 52 and 82 astronomical units from the star were detected, which alternate in
inclination with respect to the main disk.[20]
Observations in 2004 revealed the presence of an inner belt containing silicate material at a distance
of 6.4 AU from the star. Silicate material was also detected at 16 and 30 AU from the star, with a lack
of dust between 6.4 and 16 AU providing evidence that a massive planet may be orbiting in this
region.[48][49] Magnesium-rich olivine has also been detected,
strikingly similar to that found in the Solar System comets and
different from the olivine found in Solar System asteroids.[50]
Olivine crystals can only form closer than 10 AU from the star;
therefore they have been transported to the belt after formation,
probably by radial mixing.[50]
Modeling of the dust disk at 100 AU from the star suggests the
dust in this region may have been produced by a series of
collisions initiated by the destruction of planetesimals with radii of
about 180 kilometers. After the initial collision, the debris
undergoes further collisions in a process called a collisional
cascade. Similar processes have been inferred in the debris disks
around Fomalhaut and AU Microscopii.[51]
The dust around Beta Pictoris may
be produced by the collisions of
large planetesimals.
Falling evaporating bodies
The spectrum of Beta Pictoris shows strong short-term variability that was first noticed in the redshifted part of various absorption lines, which was interpreted as being caused by material falling onto
the star.[52] The source of this material was suggested to be small comet-like objects on orbits which
take them close to the star where they begin to evaporate, termed the "falling evaporating bodies"
model.[21] Transient blue-shifted absorption events were also detected, though less frequently: these
may represent a second group of objects on a different set of orbits.[53] Detailed modeling indicates
the falling evaporating bodies are unlikely to be mainly icy like comets, but instead are probably
composed of a mixed dust and ice core with a crust of refractory material.[54] These objects may have
been perturbed onto their star-grazing orbits by the gravitational influence of a planet in a mildly
eccentric orbit around Beta Pictoris at a distance of roughly 10 AU from the star.[55] Falling
evaporating bodies may also be responsible for the presence of gas located high above the plane of the
main debris disk.[56] A study from 2019 reported transiting exocomets with TESS. The dips are
asymmetric in nature and are consistent with models of evaporating comets crossing the disc of the
star. The comets are in a highly eccentric orbit and are non-periodic.[57]
Planetary system
On November 21, 2008, it was announced that infrared observations made in 2003 with the Very
Large Telescope had revealed a candidate planetary companion to the star.[58] In the autumn of 2009
the planet was successfully observed on the other side of the parent star, confirming the existence of
the planet itself and earlier observations. It is believed that in 15 years (As of 2009) it will be possible
to record the whole orbit of the planet.[14]
The European Southern Observatory confirmed the presence of Beta Pictoris c, on 6 October 2020,
through the use of direct imagery. Beta Pictoris c is orbiting in the plane of the debris disk
surrounding the star. Beta Pictoris c is currently the closest extrasolar planet to its star ever
photographed: the observed separation is roughly the same as the distance between the asteroid belt
and the Sun.[15][59]
Artistic rendering of the Beta Pictoris
system, showing accretion disk and
Beta Pictoris b and Beta Pictoris c.
The motion of Beta Pictoris b. The
orbital plane is viewed side-on; the
planet is not moving towards the
star.
The Beta Pictoris planetary system[60][61]
Companion
(in order from
star)
Mass
c
10.139 −1.031 MJ
+1.175
Inner belt
b
Semimajor
axis
Orbital
period
(AU)
(years)
+0.016
+0.015
2.680 −0.015
3.266 −0.012
Eccentricity
+0.024
0.314 −0.034
6.4 AU
+2.337
11.729 −2.135 MJ
+0.082
10.018 −0.076
+0.248
23.593 −0.209
+0.007
0.106 −0.006
Inclination
+0.083
Radius
88.947 −0.091°
—
~89°
—
89.009 ± 0.012°
1.46 ± 0.01 RJ
secondary
disk
130+ AU
89 ± 1°
—
main disk
16–1450/1835 AU
89 ± 1°
—
The radial velocity method is not well suited to study A-type stars like Beta Pictoris. The very young
age of the star makes the noise even worse. Current limits derived from this method are enough to
rule out hot Jupiter-type planets more massive than 2 Jupiter masses at a distance of less than 0.05
AU from the star. For planets orbiting at 1 AU, planets with less than 9 Jupiter masses would have
evaded detection.[22][31] Therefore, to find planets in the Beta Pictoris system, astronomers look for
the effects that the planet has on the circumstellar environment.
Multiple lines of evidence suggested the existence of a massive planet orbiting in the region around 10
AU from the star: the dust-free gap between the planetesimal belts at 6.4 AU and 16 AU suggest this
region is being cleared out;[49] a planet at this distance would explain the origin of the falling
evaporating bodies,[55] and the warps and inclined rings in the inner disk suggest a massive planet on
an inclined orbit is disrupting the disk.[44][62]
The observed planet by itself cannot explain the structure of the planetesimal belts at 30 AU and 52
AU from the star. These belts might be associated with smaller planets at 25 and 44 AU, with around
0.5 and 0.1 Jupiter masses respectively.[22] Such a system of planets, if it exists, would be close to a
1:3:7 orbital resonance. It may also be that the rings in the outer disc at 500–800 AU are indirectly
caused by the influence of these planets.[22]
The
object
was
observed
at
an
angular distance of
411
milliarcseconds
from Beta Pictoris,
which corresponds to
a distance in the plane
of the sky of 8 AU. For
comparison,
the
orbital radii of the
planets Jupiter and
Beta Pictoris b in both elongations
Saturn are 5.2 AU[63]
ESO image of a planet near Beta
and
9.5
AU[64]
Pictoris
respectively. The separation in the radial direction is unknown, so
this is a lower limit on the true separation. Estimates of its mass
depend on theoretical models of planetary evolution, and predict
the object has about 8 Jupiter masses and is still cooling, with a temperature ranging from 1400 to
1600 K. These figures come with the caveat that the models have not yet been tested against real data
in the likely ranges of mass and age for the planet.
The semimajor axis is 8–9 AU and its orbital period is 17–21 years.[65] A "transit-like event" was
observed in November 1981;[66][67] this is consistent with those estimates.[65] If this is confirmed as a
true transit, the inferred radius of the transiting object is 2–4 Jupiter radii, which is larger than
predicted by theoretical models. This may indicate that it is surrounded by a large ring system or a
moon-forming disc.[67]
Confirmation of a second planet in the Beta Pictoris system was announced on 6 October 2020. The
planet has a temperature of T = 1250 ± 50 K, a dynamical mass of M = 8.89 ± 0.75 MJup,[68] and an
age of 18.5 ± 2.5 Myr.[15] It has an orbital period of about 1,200 days (3.3 years) and a semimajor axis
of 2.7 AU, about 3.5 times closer to its parent star than Beta Pictoris b.[69][59] The orbit of Beta
Pictoris c is moderately eccentric, with an eccentricity of 0.24.[69][59]
This planet presents data with conflict with current, as of 2020, models for planetary formation. β Pic
c is at an age where planetary formations is predicted to occur via disk instability. However the planet
orbits at a distance of 2.7 AU, which prediction says is too close for disk instability to occur. The low
apparent magnitude, of MK = 14.3 ± 0.1, suggests that it formed via core accretion.[15]
Dust stream
In 2000, observations made with the Advanced Meteor Orbit Radar facility in New Zealand revealed
the presence of a stream of particles coming from the direction of Beta Pictoris, which may be a
dominant source of interstellar meteoroids in the Solar System.[23] The particles in the Beta Pictoris
dust stream are relatively large, with radii exceeding 20 micrometers, and their velocities suggest that
they must have left the Beta Pictoris system at roughly 25 km/s. These particles may have been ejected
from the Beta Pictoris debris disk as a result of the migration of gas giant planets within the disk and
may be an indication that the Beta Pictoris system is forming an Oort cloud.[70] Numerical modeling
of dust ejection indicates radiation pressure may also be responsible and suggests that planets further
than about 1 AU from the star cannot directly cause the dust stream.[71]
See also
51 Ophiuchi
Notes
1. The parallax can be converted into distance using the equation:
.
See the article on propagation of uncertainty for information on how errors on derived values can
be calculated.
2. For artist's impression of Beta Pictoris b, see:
"Length of Exoplanet Day Measured for First Time" (http://www.eso.org/public/news/eso1414/).
ESO Press Release. Retrieved 2 May 2014.
3. Calculated from [M/H]: relative abundance = 10[M/H]
4. The visual luminosity can be calculated by:
5. The physical diameter can be found by multiplying the distance by the angular diameter in
radians.
6. The rotation period can be calculated using the equations of circular motion:
7. For artist's impression of Beta Pictoris, see:
"Crashing Comets Explain Surprise Gas Clump Around Young Star" (http://www.eso.org/publi
c/news/eso1408/). ESO. Retrieved 12 March 2014.
8. From Wien's displacement law and a temperature of 8052 K the peak wavelength emission from
Beta Pictoris would be around 360 nanometers which is in the near-ultraviolet region of the
spectrum.
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External links
The Circumstellar Disk Learning Site (https://web.archive.org/web/20141104102034/http://www.dis
ksite.com/)
Beta Pictoris (https://web.archive.org/web/20081011114219/http://www.astro.uiuc.edu/~kaler/sow/
betapic.html)
Dr. David Jewitt's page on Beta Pic (http://www2.ess.ucla.edu/~jewitt/beta.html)
Beta Pictoris (http://www.solstation.com/stars2/beta-pic.htm) at SolStation.
ARICNS (https://web.archive.org/web/20060827003246/http://www.ari.uni-heidelberg.de/aricns/cn
spages/4c00467.htm)
SEDS entry (https://web.archive.org/web/20051209011731/http://www.seds.org/~spider/spider/Mis
c/betaPic.html)
Notes for star Beta Pictoris (http://exoplanet.eu/star.php?st=beta+Pic)
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