Nandan Joshi

PhD Student in Astrophysics

About Me

I am Nandan Chandrakant Joshi and was born in Mumbai(Bombay), India. I graduated with Diplom(Physik) degree from Universität Göttingen. And I’m presently pursuing a PhD in Astrophysics at the Institut für Astrophysik Göttingen.

During my graduation, I acquired substantial experience and skills in various fields of physics through praticals and research assistanceship. My research was primarily oriented in the field of optics. I also have an extensive experience in teaching in the form of practicals and tutorials.

I keep interest in all subject, whether it be politics or religion. I like to exchange thoughts and enrich my own knowledge. My personal interests are international affairs, technology, world economy, geographical philosophy, etc. I like adventure, traveling, meeting new people.

• Present
• Past

Present work

• Stellar rotation, the very cause of the generation of magnetic field, induces activity in the stars. This type of rotation-activity relation has been found sustainable for the stars with outer convective envelope. The vigor of this relation is clear for the solar-type stars, but for the stars with deeper outer convective layer or for the fully-convective stars, the clarity of this relation becomes feeble. The main reason has been that the rotational braking, defined by Skumanich, for main-sequence stars found to be inconsistent for fully-convective stars. Therefore, my main objective is to study the sample of stars in the spectral regime from early- to mid-type M-dwarfs for rotation-activity relation. This spectral regime coincides with the mass range for main sequence stars describing the transition from partial to full convection. This research project shall shed more light on whether the rotation-activity relation is consistent with the stars obeying different rotational braking mechanism.

• Present
• Past

Past work

• Stellar rotation, the very cause of the generation of magnetic field, induces activity in the stars. This type of rotation-activity relation has been found sustainable for the stars with outer convective envelope. The vigor of this relation is clear for the solar-type stars, but for the stars with deeper outer convective layer or for the fully-convective stars, the clarity of this relation becomes feeble. The main reason has been that the rotational braking, defined by Skumanich, for main-sequence stars found to be inconsistent for fully-convective stars. Therefore, my main objective is to study the sample of stars in the spectral regime from early- to mid-type M-dwarfs for rotation-activity relation. This spectral regime coincides with the mass range for main sequence stars describing the transition from partial to full convection. This research project shall shed more light on whether the rotation-activity relation is consistent with the stars obeying different rotational braking mechanism.

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• Blog calculi.isgreat.org
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