Asteroseismology in the BINA context Anwesh Mazumdar 1 , Bhaswati Mookerjea 2 , Pritesh Ranadive 1 1 Homi Bhabha Centre for Science Education (TIFR) V. N. Purav Marg, Mumbai 400088, India. 2 Dept. of Astronomy and Astrophysics, Tata Institute of Fundamental Research Homi Bhabha Road, Mumbai 400005, India. Abstract: The scope of asteroseismic studies within the Belgo-Indian Network for Astronomy and astrophysics (BINA) is explored. The main strands of current research in asteroseismology of solar-type stars are outlined. While it is obvious that it would be difficult to match the quality of the space-based seismic data on such stars with ground-based telescopes, the possibility of contribution to supplemental non-seismic data is considered. New calibrations of colour-temperature relations using archival data are presented. It is proposed that with similar calibrations with BINA-based photometric data in the future, it would be possible to provide accurate estimates of effective temperatures of solar-type stars that would be useful in asteroseismology of such stars. Keywords: asteroseismology – solar-type stars – photometry – colour – effective temperature 1 Introduction Asteroseismology or the study of oscillations in stars is, by far, the most powerful test of the theory of stellar interiors and stellar evolution. It is the only probe that can “pierce through the outer layers of a star and test the conditions within” (Eddington 1926). In recent years, this field has received an enormous boost due to the excellent data on minute oscillations collected by several space missions, namely, CoRoT, Kepler and TESS. Oscillations in stars appear mainly as two kinds of standing waves, characterized as p-modes and g-modes. The so-called p-modes are primarily acoustic in nature with gradient of pressure acting as the restoring force. The other type, g-modes, are internal gravity waves, where buoyancy provides the restoring force. Under certain situations, modes of mixed character may appear, which behave as g-modes near the core of the star and as p-modes in the exterior layers. The oscillations in stars can also be classified in two broad types, depending on the physics of the excitation mechanism. The comparatively larger amplitude oscillations, seen mostly in stars of higher mass, are the so-called opacity-driven oscillations. Solar-type stars, i.e., low mass main sequence stars, exhibit multimodal low amplitude oscillations which are excited by the turbulence in their outer convection zones. These are termed solar-like oscillations. Red giant stars, which also possess large convective outer layers, exhibit such stochastically driven oscillations as well. In this work we concentrate on solar-type stars which exhibit rich multi-mode oscillation spectra of low angular degree. Modes of higher degree cannot be observed in distant stars due to a geometric cancellation effect. However, it turns out that the low degree modes are most suited for probing the conditions of the central regions of stars. ”2nd Belgo-Indian Network for Astronomy & astrophysics (BINA) workshop”, held in Brussels (Belgium), 9-12 October 2018 Bulletin de la Société Royale des Sciences de Liège, Vol. 88, Actes de Colloques, 2019, p. 121 - 127