Near a neutron star, the tidal forces are again much stronger: if the rod has a tensile strength of 10,000 N and falls vertically to a neutron star of 2.1 solar masses, setting aside that it would melt, it would break at a distance of 190 km from the center, well above the surface (a neutron star typically has a radius of only about 12 km). For example, for a rod with a mass of 1 kg and a length of 1 m, and a massive body with the average density of the Earth, this maximum tensile force due to the tidal force is only 0.4 μN.ĭue to the high density, the tidal force near the surface of a white dwarf is much stronger, causing in the example a maximum tensile force of up to 0.24 N. In addition, there is a horizontal compression force toward the center.įor massive bodies with a surface, the tensile force is largest near the surface, and this maximum value is only dependent on the object and the average density of the massive body (as long as the object is small relative to the massive body). For non-uniform objects the tensile force is smaller if more mass is near the center, and up to twice as large if more mass is at the ends. This gives F = μ l m / 4 r 3, where μ is the standard gravitational parameter of the massive body, l is the length of the rod, m is rod's mass, and r is the distance to the massive body. In the gravity field due to a point mass or spherical mass, for a uniform rod oriented in the direction of gravity, the tensile force at the center is found by integration of the tidal force from the center to one of the ends. ( Learn how and when to remove this template message) ( January 2023) ( Learn how and when to remove this template message) Statements consisting only of original research should be removed.
Please improve it by verifying the claims made and adding inline citations. This section possibly contains original research. Spaghettification of a star was imaged for the first time in 2018 by researchers observing a pair of colliding galaxies approximately 150 million light-years from Earth. However, the term "spaghettification" was established well before this. Along with that, the right side of the body will be pulled to the left, and the left side of the body will be pulled to the right, horizontally compressing the person. If one were to fall into a black hole feet first, the gravity at their feet would be much stronger than at their head, causing the person to be vertically stretched. The reason this happens would be that the gravity force exerted by the singularity would be much stronger at one end of the body than the other. Stephen Hawking described the flight of a fictional astronaut who, passing within a black hole's event horizon, is "stretched like spaghetti" by the gravitational gradient (difference in gravitational force) from head to toe. Within a small region, the horizontal compression balances the vertical stretching so that a small object being spaghettified experiences no net change in volume.
In the most extreme cases, near a black hole, the stretching and compression are so powerful that no object can resist it. In astrophysics, spaghettification (sometimes referred to as the noodle effect) is the vertical stretching and horizontal compression of objects into long thin shapes (rather like spaghetti) in a very strong, non- homogeneous gravitational field.
The length of each arrow is proportional to the intensity of the tidal force at that point. In this diagram, the gravitational force originates from a source to the right. Tidal forces acting on a spherical body in a non-homogeneous gravitational field.
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