From AAS NOVA: ” A Four-Star Lightweight”

AASNOVA

Amercan Astronomical Society

16 October 2015
Susanna Kohler

1
Artist’s illustration of an example quadruple star system. The quadruple system 2M0441+2301 AabBab contains a low-mass star, two brown dwarfs, and a planetary-mass companion. [NASA/JPL-Caltech/UCLA]

An important part of exoplanet studies is the attempt to understand how planets and solar systems form. New measurements of the lowest-mass quadruple star system ever discovered are now confirming an intriguing theory: in addition to other channels, large gas planets may form in the same way that stars do.

Formation Channels

Exoplanets have been found in an enormous variety of configurations, from hot Jupiters only 0.01 AU away from their host star, to planetary-mass companions that orbit at a whopping distance of 1,000 AU.

Formation of these gas giants could occur via a number of different theorized pathways, such as growth from rocky cores close to host star, or fragmentation from instabilities far out in the protoplanetary disk. But given that the line between giant planets and brown dwarfs is somewhat fuzzy, another theory has come under consideration as well: could gas giants form out of the collapse and fragmentation of a molecular cloud, in the same way that stars form?

3
Within a few million years the light from bright stars will have boiled away this molecular cloud of gas and dust. The cloud has broken off from the Carina Nebula. Newly formed stars are visible nearby, their images reddened by blue light being preferentially scattered by the pervasive dust. This image spans about two light-years and was taken by the Hubble Space Telescope [HST] in 1999.

NASA Hubble Telescope
HST

In a recent study, Brendan Bowler and Lynne Hillenbrand (California Institute of Technology) argue that one star system, 2M0441+2301 AabBab, might actually be evidence that this channel works. 2M0441+2301 AabBab is a young (less than 3 million years old) quadruple system in the Taurus star-forming region. Bowler and Hillenbrand used the OSIRIS spectrograph on the Keck I telescope to verify the intriguing properties measured for this system.

Keck OSIRIS
Keck/OSIRIS

2
Near-IR spectra of 2M0441+2301 Aa, Ab, Ba, and Bb. The insets shows the unresolved 2MASS image of the system and the Keck/NIRC2 images of each binary subsystem. [Bowler&Hillenbrand 2015]

2MASS Telescope
2MASS telescope interior
2MASS

Keck Observatory
Keck NIRC2 Camera
Keck with NIRC2

Pair of Pairs

2M0441+2301 AabBab is what’s known as a hierarchical quadruple system: it consists of a pair of close-binary star systems that orbit each other at an enormous distance of at least 1,800 AU — which means that, if the system is only a few million years old, the binary pairs have orbited each other no more than ~20 times.

The authors’ measurements show that the first binary pair (labeled Aab, where Aa and Ab are the two stars) consists of a 200 MJup low-mass star and a 35 MJup brown dwarf. The second binary pair (Bab) consists of a 19 MJup brown dwarf and a ~10 MJup companion. This gives 2M0441+2301 AabBab a total mass of only ~0.26 solar masses, making it the lowest-mass quadruple system yet discovered.

The hierarchical structure of this system strongly suggests that it formed from the collapse and fragmentation of a molecular cloud core. What makes this system especially interesting is the span of masses involved. The low mass of the companion in Bab indicates that it’s possible to form planetary-mass companions from a cloud-fragmentation pathway — which suggests that this may also be legitimate channel to consider for the formation of massive exoplanets.
Citation

Brendan P. Bowler and Lynne A. Hillenbrand 2015 ApJ 811 L30. doi:10.1088/2041-8205/811/2/L30

See the full article here .

Please help promote STEM in your local schools.

STEM Icon

Stem Education Coalition