التفاصيل البيبلوغرافية
| العنوان: |
On the null detection of exoplanetary radio emission and magnetic field structures |
| المؤلفون: |
Hiremath, K M |
| المساهمون: |
Brun, Allan Sacha, Bouvier, Jérôme, Petit, Pasca |
| المصدر: |
CS21, The 21st Cambridge workshop on Cool Stars, Stellar Systems, and the Sun, Toulouse, France, 04-08 July 2022 |
| بيانات النشر: |
Zenodo |
| سنة النشر: |
2023 |
| المجموعة: |
Zenodo |
| مصطلحات موضوعية: |
stars, exoplanets, radio emission, magnetic diffusion, exoplanetary magnetic field structure |
| الوصف: |
Expected radio emission from the extra-solar planets due to physical phenomenon called "electron-cyclotron maser instability (ECMI)" requires two necessary conditions: right magnitude of stellar wind and existence of magnetic field structure of the planet. Assuming that stellar wind exists, in this study, we probe the second necessary condition for the existence of magnetic field structure of extra-solar planets from their observed radio fluxes. Even though observations show the null (statistically not significant) detection, it is interesting to examine whether there is any trend in the observed data such that clues regarding magnetic field structure can be obtained. Analysis of observational upto date emission of radio flux data of exoplanets from the literature survey yields the following results: (i) most of the observed planets have dimensions of solar Jupiter size whose magnetic diffusion time scales are estimated (assuming cores of all the exoplanets have similar core magnetic diffusivity of solar Jupiter ~ 3.5e+06 cm^2/sec) to be ~ million yrs, (ii) there are two types of planets with flux of radio emissions < 2 mJsky (let us call as type A) and >=2 mJsky (type B) that follow different evolutionary paths, (iii) majority of type A groups of planets orbit very close ( < 10 AU) to the host stars, while type B group of planets are distributed uniformly between 0.02 AU to 2000 AU, (iv) independent of their ages (assuming that planets have similar ages as those of host stars), type A planets emit similar (~ 1 mJsky) radio fluxes, whereas type B planets emit very high radio fluxes (200-300 mJsky) during their early life times (within few million yrs) and emit very low radio fluxes ( ~ 2-6 mJsky) during their old ages ( ~ 10 billion years) and, follow a power law decay of radio flux emission with respect to ages, (v) majority of type A planets have near zero eccentricty and type B planets have varied eccentricity distribution , (vi) from the mass-density distribution, it is found that, on average, type ... |
| نوع الوثيقة: |
conference object |
| اللغة: |
English, Old (ca.450-1100) |
| Relation: |
https://zenodo.org/communities/cs21; https://doi.org/10.5281/zenodo.7524252; https://doi.org/10.5281/zenodo.7524253; oai:zenodo.org:7524253 |
| DOI: |
10.5281/zenodo.7524253 |
| الاتاحة: |
https://doi.org/10.5281/zenodo.7524253 |
| Rights: |
info:eu-repo/semantics/openAccess ; Creative Commons Attribution 4.0 International ; https://creativecommons.org/licenses/by/4.0/legalcode |
| رقم الانضمام: |
edsbas.F7861A8E |
| قاعدة البيانات: |
BASE |