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കാർഷിക മേഖലയിൽ പുത്തൻ ഉണർവിനായി മൈക്രോ ഇറിഗേഷൻ  പദ്ധതി വരുന്നു

September 25, 2025
SABARI NEWS
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കോട്ടയം : കാർഷിക മേഖലയിൽ പുത്തൻ ഉണർവിനായി ജലസേചനവകുപ്പ് നടപ്പാക്കുന്ന മൈക്രോ ഇറിഗേഷൻ പദ്ധതിക്ക് ജില്ലയിൽ തുടക്കം കുറിക്കുന്നു. 2.15 കോടി രൂപ ചെലവിട്ട് കുറവിലങ്ങാട് ഗ്രാമപഞ്ചായത്തിലെ ജയ്ഗിരി വാർഡിലാണ് പദ്ധതി നടപ്പാക്കുന്നത്. കൃത്യമായ അളവിലുള്ള വെള്ളവും വളവും കൃത്യമായ ഇടവേളകളിൽ ചെടിയുടെ ചുവട്ടിൽ എത്തിക്കുന്ന ജലസേചന രീതിയാണ് മൈക്രോ (ഡ്രിപ്) ഇറിഗേഷൻ. കുറവിലങ്ങാട് കാളിയാർ തോട്ടം മേഖലയിലെ 47 കുടുംബങ്ങളുടെ ഉടമസ്ഥതയിലുള്ള 50 ഏക്കർ കൃഷിഭൂമിയിലെ സമ്മിശ്ര വിളകൾക്കാണ്തുടക്കത്തിൽ സൂക്ഷ്മ ജലസേചനസൗകര്യം ലഭ്യമാക്കുന്നത്.

414 thoughts on “കാർഷിക മേഖലയിൽ പുത്തൻ ഉണർവിനായി മൈക്രോ ഇറിഗേഷൻ  പദ്ധതി വരുന്നു”

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  168. A supernova explosion blows away the star’s outer layers, leaving a remnant such as the Crab Nebula. This core will suddenly collapse as its electrons are driven into its protons, forming neutrons, neutrinos, and gamma rays in a burst of electron capture and inverse beta decay. In massive stars, fusion continues until the iron core has grown so large (more than 1.4 M☉) that it can no longer support its own mass. If what remains after the outer atmosphere has been shed is less than roughly 1.4 M☉, it shrinks to a relatively tiny object about the size of Earth, known as a white dwarf. Eta Carinae is known for having undergone a supernova impostor event, the Great Eruption, in the 19th century. This process continues, with the successive stages being fueled by neon (see neon-burning process), oxygen (see oxygen-burning process), and silicon (see silicon-burning process). Particularly massive stars (exceeding 40 solar masses, like Alnilam, the central blue supergiant of Orion’s Belt) do not become red supergiants due to high mass loss.
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    This produces the separation of binaries into their two observed populations distributions. Most stars are observed to be members of binary star systems, and the properties of those binaries are the result of the conditions in which they formed. Less massive T Tauri stars follow this track to the main sequence, while more massive stars turn onto the Henyey track. These jets, in combination with radiation from nearby massive stars, may help to drive away the surrounding cloud from which the star was formed.
    A star with a larger mass burns more quickly and intensely than a smaller-mass star due to larger stars needing to burn more fuel to prevent its collapse. The specific causes of these winds remain unknown, but if they generally accompany star formation, astronomers will have to consider the implications for the early solar system. The remnant of a supernova observed in 1572, notably studied by the Danish astronomer Tycho Brahe, lies about 13,000 light-years away in the constellation Cassiopeia. All that’s left of the star is its core, now called a white dwarf, a roughly Earth-sized stellar cinder that gradually cools over billions of years. More massive stars must burn fuel at a higher rate to generate the energy that keeps them from collapsing under their own weight. In more massive stars, helium is produced in a cycle of reactions catalyzed by carbon called the carbon-nitrogen-oxygen cycle.
    Detailed observations of many binary star systems were collected by astronomers such as Friedrich Georg Wilhelm von Struve and S. Edward Pickering discovered the first spectroscopic binary in 1899 when he observed the periodic splitting of the spectral lines of the star Mizar in a 104-day period. In 1834, Friedrich Bessel observed changes in the proper motion of the star Sirius and inferred a hidden companion.
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