Discovering Gliese 229 Bab: A Brown Dwarf
Unraveling the mysteries of brown dwarfs and their atmospheres.
Jerry W. Xuan, Marshall D. Perrin, Dimitri Mawet, Heather A. Knutson, Sagnick Mukherjee, Yapeng Zhang, Kielan K. Hoch, Jason J. Wang, Julie Inglis, Nicole L. Wallack, Jean-Baptiste Ruffio
― 4 min read
Table of Contents
- Introducing Gliese 229 Bab
- Why Study Brown Dwarfs?
- The Tools of the Trade: JWST and MIRI
- The Atmosphere of Gliese 229 Bab
- The Mystery of Carbon and Oxygen Ratios
- How It Was Measured
- Findings on Temperature and Gravity
- Mixing and Movement in the Atmosphere
- Comparing with the Host Star
- The Role of Binarity
- What’s Next?
- A Little Humor
- Conclusion
- Original Source
- Reference Links
Brown Dwarfs are weird little stars that didn’t quite make it. They are not hot enough to be true stars like our Sun but too big to be just planets. Think of them as stars that hit the snooze button one too many times and never really woke up.
Introducing Gliese 229 Bab
Meet Gliese 229 Bab, a brown dwarf that’s part of a two-for-one special in the universe known as Gliese 229. It was recently discovered that Gliese 229 Bab has a twin, making it one of the few binary brown dwarf systems we know.
Why Study Brown Dwarfs?
Studying brown dwarfs can help scientists learn more about how objects in space form and change over time. They can also teach us about the Atmospheres of planets, especially those that are far away and might have life.
JWST and MIRI
The Tools of the Trade:To look at Gliese 229 Bab, astronomers used a fancy tool called the James Webb Space Telescope (JWST) and its Mid-Infrared Instrument (MIRI). This setup is like using a super-powered pair of binoculars to see things in the dark. It helps scientists understand what makes up these celestial bodies by analyzing the light they emit.
The Atmosphere of Gliese 229 Bab
With the power of MIRI, scientists studied the atmosphere of Gliese 229 Bab. They found that its atmosphere is surprisingly similar to the star it orbits, Gliese 229A. This means that they probably formed from the same cosmic material.
The Mystery of Carbon and Oxygen Ratios
One of the big puzzles in studying brown dwarfs like Gliese 229 Bab is figuring out the ratio of carbon to oxygen in their atmospheres. Some earlier studies suggested that Gliese 229 B had an unusually high carbon-to-oxygen ratio, which raised eyebrows. However, the new data seems to suggest that this might not be the case after all.
How It Was Measured
Using spectroscopy from JWST, scientists measured the light from Gliese 229 Bab and figured out what chemicals are present in its atmosphere. It’s a bit like tasting a dish and figuring out what ingredients are in it, but way more complicated.
Findings on Temperature and Gravity
The scientists also uncovered some juicy details about the temperature and gravity of Gliese 229 Bab. They found that one part of the binary system is hotter than the other, which is typical for two objects that are so close together.
Mixing and Movement in the Atmosphere
One fascinating aspect of brown dwarfs is how things mix in their atmospheres. The researchers measured vertical mixing rates, which tells them how fast different gases are shuffled around in the atmosphere. It’s similar to how a spoon mixes up a bowl of soup!
Comparing with the Host Star
In another twist, comparisons were made between the abundances of elements in Gliese 229 Bab and its host star, Gliese 229A. The results were astonishingly consistent! This similarity supports the idea that they formed together and that a lot of the stuff in brown dwarfs comes from the same place as nearby stars.
Binarity
The Role ofOne interesting question is how being in a binary system affects the atmospheres of these brown dwarfs. While many previous studies treated Gliese 229 B as a single star, this new packing of data helps clarify the effects of binarity. Turns out, it doesn’t seem to mess things up too much, keeping our understanding on track.
What’s Next?
With all these new findings, the next steps for astronomers might include using different models to interpret the data even better or looking at other brown dwarfs in a similar manner.
A Little Humor
If Gliese 229 Bab had a dating profile, it might read: “I’m just a brown dwarf looking for my other half to share starlit evenings with. Must love long orbits and cosmic phenomena!”
Conclusion
The study of Gliese 229 Bab paints a more detailed picture of brown dwarfs and their atmospheres. It helps bridge the knowledge gap between stars and planets and allows us a closer look at the fascinating world beyond our own. Who knew space could tell us so much about the ingredients of the universe, right from our own backyard?
Title: Atmospheric abundances and bulk properties of the binary brown dwarf Gliese 229 Bab from JWST/MIRI spectroscopy
Abstract: We present JWST/MIRI low-resolution spectroscopy ($4.75-14~\mu$m) of the first known substellar companion, Gliese 229 Bab, which was recently resolved into a tight binary brown dwarf. Previous atmospheric retrieval studies modeling Gliese 229 B as a single brown dwarf have reported anomalously high carbon-to-oxygen ratios (C/O) of $\approx 1.1$ using $1-5~\mu$m ground-based spectra. Here, we fit the MIRI spectrum of Gliese 229 Bab with a two-component binary model using the Sonora Elf Owl grid and additionally account for the observed $K$ band flux ratio of the binary brown dwarf. Assuming the two brown dwarfs share the same abundances, we obtain $\rm C/O=0.65\pm0.05$ and $\rm [M/H]=0.00^{+0.04}_{-0.03}$ as their abundances ($2\sigma$ statistical errors), which are fully consistent with the host star abundances. We also recover the same abundances if we fit the MIRI spectrum with a single brown dwarf model, indicating that binarity does not strongly affect inferred abundances from mid-infrared data when the $T_\rm{eff}$ are similar between components of the binary. We measure $T_\rm{eff}=900^{+78}_{-29}~$K and $T_\rm{eff}=775^{+20}_{-33}~$K for the two brown dwarfs. We find that the vertical diffusion coefficients of $\log{K_\rm{zz}} \approx4.0$ are identical between the two brown dwarfs and in line with $\log{K_\rm{zz}}$ values inferred for isolated brown dwarfs with similar $T_\rm{eff}$. Our results demonstrate the power of mid-infrared spectroscopy in providing robust atmospheric abundance measurements for brown dwarf companions and by extension, giant planets.
Authors: Jerry W. Xuan, Marshall D. Perrin, Dimitri Mawet, Heather A. Knutson, Sagnick Mukherjee, Yapeng Zhang, Kielan K. Hoch, Jason J. Wang, Julie Inglis, Nicole L. Wallack, Jean-Baptiste Ruffio
Last Update: 2024-11-15 00:00:00
Language: English
Source URL: https://arxiv.org/abs/2411.10571
Source PDF: https://arxiv.org/pdf/2411.10571
Licence: https://creativecommons.org/licenses/by/4.0/
Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.
Thank you to arxiv for use of its open access interoperability.