The Enigmatic Star TOI-396 and Its Planets
TOI-396 reveals intriguing planet interactions and structures, sparking new research.
A. Bonfanti, I. Amateis, D. Gandolfi, L. Borsato, J. A. Egger, P. E. Cubillos, D. Armstrong, I. C. Leão, M. Fridlund, B. L. Canto Martins, S. G. Sousa, J. R. De Medeiros, L. Fossati, V. Adibekyan, A. Collier Cameron, S. Grziwa, K. W. F. Lam, E. Goffo, L. D. Nielsen, F. Rodler, J. Alarcon, J. Lillo-Box, W. D. Cochran, R. Luque, S. Redfield, N. C. Santos, S. C. C. Barros, D. Bayliss, X. Dumusque, M. A. F. Keniger, J. Livingston, F. Murgas, G. Nowak, A. Osborn, H. P. Osborn, E. Pallé, C. M. Persson, L. M. Serrano, P. A. Strøm, S. Udry, P. J. Wheatley
― 4 min read
Table of Contents
- The Star and Its Planets
- Measuring Planet Sizes and Weights
- Understanding the Masses
- Unusual Planet Structure
- Stellar Activity and Its Effects
- Studying Planet Interactions
- The Search for a Missing Planet
- Atmospheric Studies with JWST
- Internal Structures of the Planets
- Future Observations and Opportunities
- Conclusion: A Cosmic Mystery
- Original Source
- Reference Links
TOI-396 is a bright star you can see without a telescope, located in the Fornax constellation. It has three small planets circling around it, which caught the attention of scientists. These planets were discovered using advanced cameras in space, and they all have similar sizes but different weights. This planetary trio offers an exciting chance to learn more about how planets form and behave.
The Star and Its Planets
TOI-396 is classified as an F-type star, similar to our Sun but a bit hotter. This star is about 31.7 light-years away from Earth, making it a neighbor in cosmic terms. The three planets orbiting this star exhibit some interesting characteristics. Two of them have orbits that are close to a specific ratio known as the 5:3 resonance, which is like a cosmic dance between them.
Measuring Planet Sizes and Weights
To understand more about these planets, scientists aimed to find out their sizes and weights. They used powerful telescopes to observe how the planets blocked some light from the star when they passed in front of it. This pass-through helps calculate their sizes and gives clues about their weights.
Understanding the Masses
The masses of these planets are tricky to figure out, but scientists can extract this information from their movements and how they affect the star. They watched how much the star wobbled due to the Gravitational pull of the planets. This wobbling provides valuable data to calculate the mass of the planets.
Unusual Planet Structure
Interestingly, the structure of these planets isn't what you'd expect. Typically, planets further from their star are denser, but one of the planets closer to TOI-396 is denser than the outer one. This oddity makes researchers think twice about how these planets formed and evolved over time.
Stellar Activity and Its Effects
Stars often have active behaviors, like sunspots and flares, which can interfere with our observations. For TOI-396, some changes linked to the star's activity might have obscured our ability to find clear signals from one of the planets. This can be similar to trying to hear someone talking while a loud concert is going on.
Studying Planet Interactions
The planets TOI-396 b and c are close enough that they interact gravitationally. This interaction leads to variations in their transit timing, known as Transit Timing Variations (TTVs). By studying these variations, scientists can learn more about their masses and behaviors.
The Search for a Missing Planet
One of the planets, TOI-396 c, is a bit elusive, and its weight was harder to measure than the others. Researchers believe that the signals from TOI-396 c might have been masked by the star’s activity. It’s as if you’re trying to find a cat hiding behind a curtain while your buddy keeps playing music to distract you.
Atmospheric Studies with JWST
Given that TOI-396 and its planets are so intriguing, scientists are excited about studying their Atmospheres using the upcoming James Webb Space Telescope (JWST). They hope to gather more information through special observations that would help distinguish between types of atmospheres, whether they are more like what we see on Earth or more exotic.
Internal Structures of the Planets
To understand what the planets are made of, researchers use models to simulate their potential internal structures. By seeing how these planets might be layered-from heavy iron cores to lighter atmospheres-scientists can make educated guesses about their compositions. It’s not unlike figuring out what’s inside a chocolate cake by looking at the layers.
Future Observations and Opportunities
The study of TOI-396 and its planets appears promising for future observations. Scientists have plans to keep a close watch on the system, maneuvering their telescopes to catch these planets in action. They anticipate new discoveries, which could offer insights into how planetary systems form and evolve.
Conclusion: A Cosmic Mystery
TOI-396 holds many secrets yet to be uncovered. As scientists continue to study this star system, they hope to piece together the complex puzzle of planetary formation and dynamics. With every observation, they come closer to answering the big questions about our universe and the fascinating worlds that inhabit it.
Title: Radii, masses, and transit-timing variations of the three-planet system orbiting the naked-eye star TOI-396
Abstract: TOI-396 is an F6V star ($V\approx6.4$) orbited by three transiting planets. The orbital periods of the two innermost planets are close to the 5:3 commensurability ($P_b \sim3.6$ d and $P_c \sim6.0$ d). To measure the masses of the three planets, refine their radii, and investigate whether planets b and c are in MMR, we carried out HARPS RV observations and retrieved photometric data from TESS. We extracted the RVs via a skew-normal fit onto the HARPS CCFs and performed an MCMC joint analysis of the Doppler measurements and transit photometry, while employing the breakpoint method to remove stellar activity from the RV time series. We also performed a thorough TTV dynamical analysis of the system. Our analysis confirms that the three planets have similar sizes: $R_b=2.004_{-0.047}^{+0.045}R_{\oplus}$; $R_c=1.979_{-0.051}^{+0.054}R_{\oplus}$; $R_d=2.001_{-0.064}^{+0.063}R_{\oplus}$. For the first time, we have determined the RV masses for TOI-396b and d: $M_b=3.55_{-0.96}^{+0.94}M_{\oplus}$ ($\rho_b=2.44_{-0.68}^{+0.69}$ g cm$^{-3}$) and $M_d=7.1\pm1.6M_{\oplus}$ ($\rho_d=4.9_{-1.1}^{+1.2}$ g cm$^{-3}$). Our results suggest a quite unusual system architecture, with the outermost planet being the densest. The Doppler reflex motion induced by TOI-396c remains undetected in our RV time series, likely due to the proximity of $P_c$ to the star's rotation period ($P_{\mathrm{rot}}=6.7\pm1.3$ d). We also discovered that TOI-396b and c display significant TTVs. While the TTV dynamical analysis returns a formally precise mass for TOI-396c ($M_{c,\mathrm{dyn}}=2.24^{+0.13}_{-0.67}M_{\oplus}$), the result might not be accurate owing to the poor sampling of the TTV phase. We also conclude that TOI-396b and c are close to but out of the 5:3 MMR. Our numerical simulation suggests TTV semi-amplitudes of up to 5 hours over a temporal baseline of $\sim$5.2 years.
Authors: A. Bonfanti, I. Amateis, D. Gandolfi, L. Borsato, J. A. Egger, P. E. Cubillos, D. Armstrong, I. C. Leão, M. Fridlund, B. L. Canto Martins, S. G. Sousa, J. R. De Medeiros, L. Fossati, V. Adibekyan, A. Collier Cameron, S. Grziwa, K. W. F. Lam, E. Goffo, L. D. Nielsen, F. Rodler, J. Alarcon, J. Lillo-Box, W. D. Cochran, R. Luque, S. Redfield, N. C. Santos, S. C. C. Barros, D. Bayliss, X. Dumusque, M. A. F. Keniger, J. Livingston, F. Murgas, G. Nowak, A. Osborn, H. P. Osborn, E. Pallé, C. M. Persson, L. M. Serrano, P. A. Strøm, S. Udry, P. J. Wheatley
Last Update: 2024-12-10 00:00:00
Language: English
Source URL: https://arxiv.org/abs/2411.14911
Source PDF: https://arxiv.org/pdf/2411.14911
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.
Reference Links
- https://orcid.org/0000-0002-1916-5935
- https://orcid.org/0000-0001-8627-9628
- https://orcid.org/0000-0003-0066-9268
- https://orcid.org/0000-0003-1628-4231
- https://orcid.org/0000-0002-1347-2600
- https://orcid.org/0000-0002-5080-4117
- https://orcid.org/0000-0001-5845-947X
- https://orcid.org/0000-0002-0855-8426
- https://orcid.org/0000-0001-5578-7400
- https://orcid.org/0000-0001-9047-2965
- https://orcid.org/0000-0001-8218-1586
- https://orcid.org/0000-0003-4426-9530
- https://orcid.org/0000-0002-0601-6199
- https://orcid.org/0000-0002-8863-7828
- https://orcid.org/0000-0003-3370-4058
- https://orcid.org/0000-0002-9910-6088
- https://orcid.org/0000-0001-9670-961X
- https://orcid.org/0000-0002-5254-2499
- https://orcid.org/0000-0003-3742-1987
- https://orcid.org/0000-0001-9662-3496
- https://orcid.org/0000-0002-4671-2957
- https://orcid.org/0000-0003-3786-3486
- https://orcid.org/0000-0003-4422-2919
- https://orcid.org/0000-0003-2434-3625
- https://orcid.org/0000-0001-6023-1335
- https://orcid.org/0000-0002-9332-2011
- https://orcid.org/0000-0002-4881-3620
- https://orcid.org/0000-0001-9087-1245
- https://orcid.org/0000-0002-7031-7754
- https://orcid.org/0000-0002-5899-7750
- https://orcid.org/0000-0002-4047-4724
- https://orcid.org/0000-0003-0987-1593
- https://orcid.org/0000-0003-1257-5146
- https://orcid.org/0000-0001-9211-3691
- https://orcid.org/0000-0001-7576-6236
- https://orcid.org/0000-0003-1452-2240
- https://www.stsci.edu/~valenti/sme.html
- https://github.com/sousasag/ARES
- https://stev.oapd.inaf.it/cgi-bin/cmd
- https://tasoc.dk/docs/EXP-TESS-ARC-ICD-TM-0014-Rev-F.pdf
- https://kurucz.harvard.edu/grids.html
- https://github.com/nespinoza/limb-darkening
- https://exoplanetarchive.ipac.caltech.edu/
- https://github.com/lucaborsato/trades
- https://emcee.readthedocs.io/en/stable/tutorials/moves/
- https://emcee.readthedocs.io/en/stable/tutorials/autocorr/
- https://heasarc.gsfc.nasa.gov/wsgi-scripts/TESS/TESS-point_Web_Tool/TESS-point_Web_Tool/wtv_v2.0.py/
- https://github.com/joannegger/plaNETic
- https://www.cosmos.esa.int/gaia
- https://www.cosmos.esa.int/web/gaia/dpac/consortium
- https://tex.stackexchange.com/questions/547412/long-table-appendix-numbering-a-b-c