Planetary Engulfment Prognosis within the ρ CrB System
Exoplanets have been detected around stars at various stages of their lives, ranging from young stars emerging from formation to the latter stages of evolution, including white dwarfs and neutron stars. Post-main-sequence stellar evolution can result in dramatic, and occasionally traumatic, alterati...
| Main Author: | |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2023-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ad06b2 |
| _version_ | 1797613801430843392 |
|---|---|
| author | Stephen R. Kane |
| author_facet | Stephen R. Kane |
| author_sort | Stephen R. Kane |
| collection | DOAJ |
| description | Exoplanets have been detected around stars at various stages of their lives, ranging from young stars emerging from formation to the latter stages of evolution, including white dwarfs and neutron stars. Post-main-sequence stellar evolution can result in dramatic, and occasionally traumatic, alterations to the planetary system architecture, such as tidal disruption of planets and engulfment by the host star. The ρ CrB system is a particularly interesting case of advanced main-sequence evolution, due to the relative late age and brightness of the host star, its similarity to solar properties, and the harboring of four known planets. Here, we use stellar evolution models to estimate the expected trajectory of the stellar properties of ρ CrB, especially over the coming 1.0–1.5 billion yr as it evolves off the main sequence. We show that the inner three planets (e, b, and c) are engulfed during the red giant phase and asymptotic giant branch, likely destroying those planets via either evaporation or tidal disruption at the fluid-body Roche limit. The outer planet, planet d, is briefly engulfed by the star several times toward the end of the asymptotic giant branch, but the stellar mass loss and subsequent changing planetary orbit may allow the survival of the planet into the white dwarf phase of the stellar evolution. We discuss the implications of this outcome for similar systems and describe the consequences for planets that may lie within the habitable zone of the system. |
| first_indexed | 2024-03-11T06:59:46Z |
| format | Article |
| id | doaj.art-9e5b75fae835464f985a39eb8bbd24ea |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T06:59:46Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-9e5b75fae835464f985a39eb8bbd24ea2023-11-17T09:20:57ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01958212010.3847/1538-4357/ad06b2Planetary Engulfment Prognosis within the ρ CrB SystemStephen R. Kane0https://orcid.org/0000-0002-7084-0529Department of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USA ; skane@ucr.eduExoplanets have been detected around stars at various stages of their lives, ranging from young stars emerging from formation to the latter stages of evolution, including white dwarfs and neutron stars. Post-main-sequence stellar evolution can result in dramatic, and occasionally traumatic, alterations to the planetary system architecture, such as tidal disruption of planets and engulfment by the host star. The ρ CrB system is a particularly interesting case of advanced main-sequence evolution, due to the relative late age and brightness of the host star, its similarity to solar properties, and the harboring of four known planets. Here, we use stellar evolution models to estimate the expected trajectory of the stellar properties of ρ CrB, especially over the coming 1.0–1.5 billion yr as it evolves off the main sequence. We show that the inner three planets (e, b, and c) are engulfed during the red giant phase and asymptotic giant branch, likely destroying those planets via either evaporation or tidal disruption at the fluid-body Roche limit. The outer planet, planet d, is briefly engulfed by the star several times toward the end of the asymptotic giant branch, but the stellar mass loss and subsequent changing planetary orbit may allow the survival of the planet into the white dwarf phase of the stellar evolution. We discuss the implications of this outcome for similar systems and describe the consequences for planets that may lie within the habitable zone of the system.https://doi.org/10.3847/1538-4357/ad06b2ExoplanetsAstrobiologyHabitable zoneStellar evolutionStellar evolutionary modelsExpanding stellar envelopes |
| spellingShingle | Stephen R. Kane Planetary Engulfment Prognosis within the ρ CrB System The Astrophysical Journal Exoplanets Astrobiology Habitable zone Stellar evolution Stellar evolutionary models Expanding stellar envelopes |
| title | Planetary Engulfment Prognosis within the ρ CrB System |
| title_full | Planetary Engulfment Prognosis within the ρ CrB System |
| title_fullStr | Planetary Engulfment Prognosis within the ρ CrB System |
| title_full_unstemmed | Planetary Engulfment Prognosis within the ρ CrB System |
| title_short | Planetary Engulfment Prognosis within the ρ CrB System |
| title_sort | planetary engulfment prognosis within the ρ crb system |
| topic | Exoplanets Astrobiology Habitable zone Stellar evolution Stellar evolutionary models Expanding stellar envelopes |
| url | https://doi.org/10.3847/1538-4357/ad06b2 |
| work_keys_str_mv | AT stephenrkane planetaryengulfmentprognosiswithinthercrbsystem |