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🌿 4월 건강 정보 안내

안녕하세요 :)

NGO 사랑해 지킴이 LOVE 입니다.

나른한 이 계절, 나는 괜찮나요?

요즘 유난히 몸이 무겁고,

이유 없이 무기력하게 느껴지시나요?

단순한 피로가 아니라

계절성 우울증일 수도 있습니다.

계절성 우울증은

계절 변화에 따라 반복적으로 나타나는 우울 증상으로,

신체 리듬의 변화로 인해 발생할 수 있어요.

✔ 우울감, 불안감

✔ 과다수면

✔ 식욕 증가

✔ 집중력 저하

이런 변화가 느껴진다면

내 마음의 상태를 한 번 돌아보는 것이 필요합니다.

🌤 왜 이런 증상이 나타날까요?

-일조량의 변화

-호르몬 변화

-외부 환경 요인

특히 햇빛이 줄어들면

기분을 안정시키는 호르몬 균형이 흔들릴 수 있습니다.

🌱 이렇게 극복해보세요!

☀ 따뜻한 햇빛 받기

하루 20~30분 햇빛을 쬐면

기분을 안정시키는 호르몬이 활성화되어

우울감 완화에 도움을 줄 수 있어요.

🚶‍♀️ 가벼운 운동하기

걷기나 스트레칭 같은 가벼운 운동은

몸의 긴장을 풀어주고 기분을 좋게 만들어줍니다.

⚠ 꼭 기억해주세요

시간이 지나면서 자연스럽게 나아질 수도 있지만,

이러한 상태가 2주 이상 지속된다면

전문기관의 도움을 받는 것이 중요합니다.

계절의 변화만큼

우리의 마음도 영향을 받을 수 있습니다.

괜찮은 척하기보다,

나의 상태를 살피는 것부터 시작해보세요.

NGO 사랑해는

여러분의 마음이 건강하게 회복될 수 있도록 함께하겠습니다 💛

#NGO사랑해 #계절성우울증 #마음건강 #봄철우울 #자기돌봄

✨ 마음이 힘들 때, NGO 사랑해는 언제나 당신의 편입니다.👉도움받기

후원하기👉 하나은행 261-910038-34304 (예금주: 사랑해)

더욱 더 열심히하는 NGO사랑해 가 되겠습니다.

🧸 자세한 사항은 공식홈페이지, 인스타그램, 트위터, 페이스북 등 확인 할 수 있어요

궁금하신 사항은 언제든 💌 쪽지 부탁드립니다.

Theda Chiu2026-05-17 11:31

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. The star then follows an evolutionary path called the asymptotic giant branch (AGB) that parallels the other described red-giant phase, but with a higher luminosity. In about 5 billion years, when the Sun enters the helium burning phase, it will expand to a maximum radius of roughly 1 astronomical unit (150 million kilometres), 250 times its present size, and lose 30% of its current mass. A star's metallicity can influence the time the star takes to burn its fuel, and controls the formation of its magnetic fields, which affects the strength of its stellar wind.
The time a star spends on the main sequence depends primarily on the amount of fuel it has and the rate at which it fuses it. However, very massive stars can lose 10−7 to 10−5 M☉ each year, significantly affecting their evolution. Stars spend about 90% of their lifetimes fusing hydrogen into helium in high-temperature-and-pressure reactions in their cores. 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.
The more massive the star, the shorter its lifespan, primarily because massive stars have greater pressure on their cores, causing them to burn hydrogen more rapidly. Some stars may even be close to 13.8 billion years old—the observed age of the universe. Almost everything about a star is determined by its initial mass, including such characteristics as luminosity, size, evolution, lifespan, and its eventual fate. In a 2017 study of the Perseus molecular cloud, astronomers found that most of the newly formed stars are in binary systems. Many stars are observed, and most or all may have originally formed in gravitationally bound, multiple-star systems.
Some low-mass stars will shine for trillions of years – longer than the universe has currently existed – while some massive stars will live for only a few million years. Our Sun, a main sequence star, emits a strong solar flare flashes in this image captured by NASA's Solar Dynamics Observatory. Nuclear fusion releases energy, which heats the star and prevents it from further collapsing under the force of gravity. After millions of years, immense pressures and temperatures in the star’s core squeeze the nuclei of hydrogen atoms together to form helium, a process called nuclear fusion.
Molecular clouds are giant, spanning hundreds of light years in size and ranging from 1,000 to 10 million times the size of our Sun. Black Holes Might be Defects in Space and TimeBlack holes are singularities in space with gravitational pulls so strong that nothing can escape from within them. According to NASA, astronomers estimate there could be as many as one septillion stars in the universe, which is a one with 24 zeros after it. 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.
Medieval Islamic astronomers gave Arabic names to many stars that are still used today and they invented numerous astronomical instruments that could compute the positions of the stars. In 185 AD, they were the first to observe and write about a supernova, now known as SN 185. Despite the apparent immutability of the heavens, Chinese astronomers were aware that new stars could appear. The earliest known star catalogues were compiled by the ancient Babylonian astronomers of Mesopotamia in the late 2nd millennium BC, during the Kassite Period (c. 1531 BC – c. 1155 BC).
Mass transfer through gravitational stripping in binary systems is seen by some astronomers as the solution to that problem. The outflow from supernovae and the stellar wind of large stars play an important part in shaping the interstellar medium. The core is compressed into a neutron star, which sometimes manifests itself as a pulsar or X-ray burster. 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.
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