Star Formation: La formación de estrellas
Step1: A condensation of gas, dust, and ice come together to make what is called a nebula.
Step2: These clouds of dust put a gravitational force on each other cause them to attract together.
Step3: The gravitational instability within the nebula causes them to break apart but into smaller parts.
Step4: As they get smaller then the temperature gets hotter. When the temperature reaches 1 million K, the center of the cloud is a protostar. When the temperature reaches 10 million K, hydrogen fuses to form helium and a star is created.
Step2: These clouds of dust put a gravitational force on each other cause them to attract together.
Step3: The gravitational instability within the nebula causes them to break apart but into smaller parts.
Step4: As they get smaller then the temperature gets hotter. When the temperature reaches 1 million K, the center of the cloud is a protostar. When the temperature reaches 10 million K, hydrogen fuses to form helium and a star is created.
HR Charts: Tablas de recursos humanos
Hertzsprung- Russell(HR) charts or sometimes called diagrams were invented in the early 1900's by Ejnar Hertzsprung and Henry Russell. They studied the relationship between absolute magnitude and temperature of stars. The higher- temperature stars radiate more energy and have higher absolute magnitudes. Even unformed stars like protostars can be plotted on the diagram. About 90% of stars fall in the main sequence and the other 10% fall elsewhere.
On the diagram, the colors go from white to blue to yellow to orange to red from white being the hottest and red being the coolest. Luminosity( brightness) is located on the vertical( Y) axis and temperature is located on the horizontal ( X) axis.
Types of stars
Main Sequence: To stay on the main sequence, the star's gravity balance outward pressures. Stars stay on the main sequence for most of their life. For example, the Sun has been on the main sequence for 5 billion years and will continue for another 5 billion years. When hydrogen fuel has ran out, a stars loses it main sequence status. Next, the star is classed by the total mass of the star. An average star will become a giant, then a white dwarf, and finally a black dwarf. More massive stars can become supergiants and end up as neutron stars or black holes. Stars below average could remain on the main sequence for 16 trillion years. The most common stars on the main sequence are red dwarfs which make up about 80% of all stars.
Main Sequence: To stay on the main sequence, the star's gravity balance outward pressures. Stars stay on the main sequence for most of their life. For example, the Sun has been on the main sequence for 5 billion years and will continue for another 5 billion years. When hydrogen fuel has ran out, a stars loses it main sequence status. Next, the star is classed by the total mass of the star. An average star will become a giant, then a white dwarf, and finally a black dwarf. More massive stars can become supergiants and end up as neutron stars or black holes. Stars below average could remain on the main sequence for 16 trillion years. The most common stars on the main sequence are red dwarfs which make up about 80% of all stars.
Giants and Dwarfs: When all of the hydrogen is consumed in the core of a star, its outward pressure is overcome by gravity. Its core increases in temperature and contracts and the outer layers are cooled. It is now considered a giant in this late stage. The core continues to contract and become hotter until the cores uses up all the helium and contracts more. When the temperature rises up to 100 million K, helium fuses while forming carbon. The star is gigantic and its outer surface is much cooler but its outer layers shed only leaving the hot, dense core. It is now a white dwarf.
Supernovas, Neutron Stars, and Black Holes: The more massive stars( larger than our Sun) are different than the average stars. Their cores are very hot and reach temperatures that cause fusion to produce heavier elements. The star starts in a supergiant, then iron takes up the core but iron does not fuse properly so there is no outward radiation of energy to neutralize the inward pull of gravity. The core collapses harshly and the our portion of the star booms, and causes a supernova. A supernova, an enormous explosion, is when the temperature in the core is 10 billion K and atomic nuclei are split into neutrons and protons. Protons come together to make neutrons and the core become a neutron star. Tremendous stars are more different. In their final stage, the last collapse of the core skips the neutron-star stage and becomes a black hole. A black hole is an object so dense that if an object got too close it would suck it right up because of its gravitational force.
Supernovas: Previously said, supernovas are enormous explosions. They are two types of supernovas: Type 1 and Type 2. Type 1 supernovas are formed from low hydrogen and low mass stars that have pulled matter in from a close red giant star. Then the process carbon denotation causes carbon fusion almost everywhere inside the star and is theorized to damage the star completely. Type 2 supernovas form from hydrogen rich, high mass stars. They only leave a collapsed core that can reduce into a neutron star or black hole.
Supernovas, Neutron Stars, and Black Holes: The more massive stars( larger than our Sun) are different than the average stars. Their cores are very hot and reach temperatures that cause fusion to produce heavier elements. The star starts in a supergiant, then iron takes up the core but iron does not fuse properly so there is no outward radiation of energy to neutralize the inward pull of gravity. The core collapses harshly and the our portion of the star booms, and causes a supernova. A supernova, an enormous explosion, is when the temperature in the core is 10 billion K and atomic nuclei are split into neutrons and protons. Protons come together to make neutrons and the core become a neutron star. Tremendous stars are more different. In their final stage, the last collapse of the core skips the neutron-star stage and becomes a black hole. A black hole is an object so dense that if an object got too close it would suck it right up because of its gravitational force.
Supernovas: Previously said, supernovas are enormous explosions. They are two types of supernovas: Type 1 and Type 2. Type 1 supernovas are formed from low hydrogen and low mass stars that have pulled matter in from a close red giant star. Then the process carbon denotation causes carbon fusion almost everywhere inside the star and is theorized to damage the star completely. Type 2 supernovas form from hydrogen rich, high mass stars. They only leave a collapsed core that can reduce into a neutron star or black hole.
Spectral Class :Espectral Clase
Stars are classified by their spectra and temperature. They are 7 different types going hottest to coolest: O, B, A, F, G, K, and M. M is common and dim, and O and B are uncommon, but bright. The HR Diagrams plot the stars on their temperature vs their luminosity. The spectral class is a way of classifying stars by their characteristics.
Stars are classified by their spectra and temperature. They are 7 different types going hottest to coolest: O, B, A, F, G, K, and M. M is common and dim, and O and B are uncommon, but bright. The HR Diagrams plot the stars on their temperature vs their luminosity. The spectral class is a way of classifying stars by their characteristics.
Q1: Where on the HR Diagram will you find white dwarfs?
Q2: On the HR Diagram, what category do the most common stars fall into?
Q3: What temperature does hydrogen fuse to create helium and star is born?
Q4: What are stars classed by?
Q5: What do black holes do?