About Me

I am from a remote village in West Bengal. I work at the Physical Research Laboratory (PRL) in Ahmedabad. Besides PRL, I also worked in The University of Virginia, S N Bose National Centre for Basic Sciecnes, and Leiden Observatory. Besides my work, I love reading and classical music.

Contact Details

Kinsuk Acharyya
Navrangpura, Ahmedabad, 380009
Gujarat, India

Phone:+91(0)7926314521 (office)
Email:[email protected] (office)
[email protected] (personal)

Publications

Recent Publications

  • K. Acharyya,``Understanding the impact of diffusion of CO in the astrochemical models", 2022, PASA, 39, 9
  • J. P. Pabari, J. P., S. Nambiar, R. K. Singh, A. Bhardwaj, K. A. Lad, K. Acharyya et. al. ``IDP detection in Earth environment: Prediction of plasma capture efficiency and detector response to high-energy particles" 2022, PSS, 215, 105452
  • S. Ahmed and K. Acharyya, 'Gas phase modeling of the cometary coma of interstellar comet 2I/Borisov', 2021, 923, 91 ApJ
  • V. R. Dinesh Kumar, J. P. Pabari, K. Acharyya, and C. T., `Venus lightning: Estimation of charge and dimensions of charge regions for lightning initiation', 2021, Icarus, 365, 114473
  • S. Nickerson, N. Rangwala, S. Colgan, C. DeWitt, X. Huang, K. Acharyya, et al., ‘The First Mid-Infrared Detection of HNC in the Interstellar Medium: Probing the Extreme Environment Towards the Orion Hot Core’, 2021, ApJ, 907, 51
  • K. Acharyya, Sean W. Schulte, and E. Herbst, ``The Effect of Chemisorption on the Chemical Evolution of Star-forming Regions", 2020, 247, 4
  • K. Acharyya, and E. Herbst, 2018, ''Hot Cores in Magellanic Clouds", ApJ, 2018, 859, 51
  • N. Rangwala, S. W. J. Colgan, R. Le Gal, K. Acharyya, X. Huang, et al., 2018, ''High Spectral Resolution SOFIA/EXES Observations of C2H2 toward Orion IRc2 ", ApJ, 2018, 856, 9
  • K. Acharyya, and E. Herbst, 2017, ''Gas-grain Fluorine and Chlorine Chemistry in the Interstellar Medium", ApJ, 2017, 850, 105
  • Jiao, He., K. Acharyya, and Vidali, G., 2016, ''Binding Energy of Molecules on Water Ice: Laboratory Measurements and Modeling", ApJ, 2016, 825, 89
  • Jiao, He., K. Acharyya, and Vidali, G., 2016, ``Sticking of molecules on non-porous amorphous water ice", ApJ, 2016, 823, 56
  • K. Acharyya, E. Herbst, 2016,``Simulations of the Chemistry in the Small Magellanic Cloud", ApJ, 822, 105
  • K. Acharyya and E. Herbst, 2015, ``Molecular Development in the Large Magellanic Cloud", ApJ, 812, 142
  • K. Acharyya, E. Herbst, R. L. Caravan, R. J. Shannon, M. A. Blitz \& D. E. Heard, 2015, `` The importance of OH radical–neutral low temperature tunnelling reactions in interstellar clouds using a new model", Molecular Physics, 113, 2243
  • Few Selected Publications before 2015

  • K. Acharyya, 2014, "Laboratory study of sticking and desorption of H2 and its significance in the chemical evolution of dense interstellar medium", MNRAS, 443, 1301
  • W. Iqbal, K Acharyya, and E. Herbst, 2014, "Effect of size distribution and diverse surfaces on H2 Formation in Diffuse Clouds studied by Kinetic Monte Carlo Approach", ApJ, 784, 139
  • Umut A. Yıldız, Kinsuk Acharyya, Paul F. Goldsmith, Ewine F. van Dishoeck, Gary Melnick, and et al., 2013, "Deep observations of O2 toward a low-mass protostar with Herschel-HIFI", Astronomy and Astrophysics, 558, 58
  • W. Iqbal, K. Acharyya, and E. Herbst, 2012, "Kinetic Monte Carlo Studies of H2 Formation on Grains Surfaces over a Wide Temperature Range", ApJ, 751, 58
  • K. Acharyya, G. Hassel, and E. Herbst, 2011, "Effect of grain sizes and grain growth on the chemical evolution of dense cloud", ApJ, 732, 72
  • A. Das, K. Acharyya, and S. K. Chakrabarti, 2010, "Effects of initial condition and cloud density on the composition of the grain mantle", MNRAS, 409, 789
  • A. Das, K. Acharyya, and S. K. Chakrabarti, 2008, "Formation of Water and Methanol in Star Forming Molecular Clouds", Astronomy and Astrophysics, 486, 209
  • K. Acharyya, G.W. Fuchs, H.J. Fraser, E.F. van Dishoeck and H. Linnartz, 2007, "Desorption rates and sticking co-efficients for CO and O2 interstellar ices", Astronomy and Astrophysics, 466, 1005
  • K. Acharyya, S. K. Chakrabarti and S. Chakrabarti, 2005, "Molecular Hydrogen Formation During Interstellar Cloud Collapse", M.N.R.A.S., 361, 550A
  • S. K. Chakrabarti, K. Acharyya, D. Molteni, 2004, "The Effect of Cooling on Time Dependent Behaviour of Accretion Flows Around Black Holes", Astronomy and Astrophysics, 421, 1C
  • S. K. Chakrabarti, K. Acharya, B. Bose, S. Mandal, A. Chatterjee, N. M. NANDI, S. PAL, R. KHAN, 2002, "Monitoring of Sudden Ionospheric Disturbances (SID) from Kolkata", Ind. J. Phys.
  • D. Molteni, K. Acharya, O. Kuznetsov, D. Bisikalo, S. K. Chakrabarti, "Kelvin-Helmholtz Instability on the Accretion Disk Surface", 2001, ApJL, v 563, p L57
  • Research Works

    Summary

    The vast space between the stars is called the Interstellar Medium (ISM). It primarily consists of a tenuous gas, small sub-micron particles called grains and energetic radiations. The local concentration of matter in ISM is called cloud. These clouds are the sites of active star formation. In addition, these clouds also shield interstellar radiation field and allow a rich chemistry to occur. Which results in formation of complex molecules (in astrophysical context molecules with six or more atoms is considered as a complex). These molecules range in complexity from diatomic H2 to a 15-atom linear nitrile, HC13N and many of these molecules are unusual to find in ISM by terrestrial standards. H2 is the most abundant molecule by far, with CO in the second position, nearly four order of magnitude lower. More complex molecules are at least 4 to 10 orders of magnitude lower than H2. Solar systems like ours are evolved in the ISM, therefore the study of generation mechanisms of these molecules in the ultra cold and ultra high vacuum conditions of ISM is of paramount importance. Analysis of cometary ices and meteoritic material also shows remarkable similarity with the interstellar ices. Thus study of the chemical evolution of ISM gives an insight to the primordial composition of our planet Earth, thereby addressing the issue how life originated on Earth. In the last few decades, it has become clear that gas phase reactions alone can not explain the molecular abundance in the ISM. The chemical reactions that occur on interstellar dust grains are needed to explain for the formation of several molecules, if not all. The dust grain surface, plays a key role as catalytic site in the formation of these molecular species. The research work aims to study the formation of complex organics in the star forming region with a combination of two lines of research:

  • The formation of complex molecules during star formation with the help of numerical simulation and
  • The laboratory study of interstellar ice analogs and formation of molecules. Which will be performed by using a state-of-the-art laboratory which can simulate dense interstellar environment
  • Current Research Interest

    Using Numerical Simulation

    a. Effect of metallicity on Chemical Complexity
    b. Effect of grain growth and grain size distribution in the formation of molecules
    c. Formation of water and prebiotic molecules in astrophysical environments
    d. Effect of physical parameters in formation of complex molecules
    e. Study of isotopic fractionation in the star forming regions
    f. Study of cometary atmosphere
    g. Understaning the atmosphere of Exoplanets

    Using Laboratory Experiments

    a. Measurement of the binding energies
    b. Understanding of desorption kinetics
    c. Measurement of sticking co-efficients
    d. Study of photo-desorption and photo processing
    e. Study of formation of Molecules

    Course Work

    Important information e.g., syllabus, assignments, exam date etc. related to the my part of the course work will be found here. Please do not hesitate to inform incase you found any inconsistency (Links are active only during the course Work).

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    Syllabus

    First Assignment

    2nd Assignment Solution

    3rd Assignment

    4th Assignment

    5th Assignment

    Exam Date -

    For any class related queries you can write me at [email protected]

    Acknowledgements

    Background image (at the top) is of famous horse head nebula which is nearly 1500 light year away. It is a region in which low-mass stars are forimg. How molecules are formed in these regions is an active topic of research. Image credit: NASA, ESA and the Hubble heritage team.
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