Hole Type
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Hole Type
Black Holes
Basics
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Basics
Types
Anatomy
Gallery
This simulation shows a black hole distorting a starry background. Credit: NASA’s Goddard Space Flight Center; background, ESA/Gaia/DPAC more
A swirling vortex of hot gas glows in this multiwavelength composite, marking the approximate location of the supermassive black hole Sagittarius A* (pronounced ey-star) at the heart of our Milky Way galaxy. Credit: NASA, ESA, SSC, CXC, STScI
Gas glows brightly in this computer simulation of supermassive black holes only 40 orbits from merging. Models like this may eventually help scientists pinpoint real examples of these powerful binary systems. Credit: NASA’s Goddard Space Flight Center/Scott Noble
NASA’s newest X-ray eyes are open and ready for discovery.
NASA’s IXPE mission launched Thursday, December 9, 2021, NASA’s Kennedy Space Center in Florida.
NASA’s Roman will use its microlensing survey to provide the best opportunity yet to definitively detect solitary small black holes.
Black holes are some of the most bizarre and fascinating objects in the cosmos – but they're invisible!
For the first time, scientists mapped out the invisible magnetic fields pulsing through Centaurus A using infrared light.
An international team of astronomers discovered a cosmic equivalent to Yellow Stone's Old Faithful geyser.
After more than 16 years studying the universe in infrared light, NASA's Spitzer mission has come to an end.
For the first time, NASA’s TESS watched a black hole tear apart a star.
NuSTAR’s observations of an ultraluminous X-ray source offer possible explanations for these mysterious objects.
Since its launch, NASA’s Spitzer has lifted the veil on the wonders of the cosmos using infrared light.
By combining NASA Chandra data with the EHT image, scientists can learn more about the giant black hole M87* and its behavior.
Scientists charted the environment surrounding a stellar-mass black hole using NASA’s NICER.
Did you know our Milky Way galaxy is blowing bubbles? Two of them, each 25,000 light-years tall!
For the first time, scientists using NASA’s Fermi found the source of a high-energy neutrino from outside our galaxy.
NASA’s Chandra data were critical in determining if a neutron star merger created a heavier neutron star or black hole.
NuSTAR identified two gas-enshrouded supermassive black holes at the centers of nearby galaxies.
These data from NASA’s Chandra gave astronomers a look at the growth of black holes over billions of years.
NASA's Swift and NuSTAR caught a supermassive black hole in the midst of a giant eruption of X-ray light.
Astronomers used NASA’s Swift satellite to detect the awakening of a distant galaxy's dormant black hole.
NASA's Fermi unveiled a previously unseen structure centered in the Milky Way.
NASA scientists have, for the first time, detected and pinned down the location of a short gamma-ray burst.
NASA Chandra data has shown ripples in the hot gas that fills the Perseus cluster are sound waves.
Hubble found seemingly conclusive evidence for a massive black hole in the center of the giant elliptical galaxy M87.
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This site is maintained by the Astrophysics Communications teams at NASA's Goddard Space Flight Center and NASA's Jet Propulsion Laboratory for NASA's Science Mission Directorate.
Astronomers generally divide black holes into three categories according to their mass: stellar-mass, supermassive, and intermediate-mass. The mass ranges that define each group are approximate, and scientists are always reassessing where the boundaries should be set. Cosmologists suspect a fourth type, primordial black holes formed during the birth of the universe, may also lurk undetected in the cosmos.
When a star with more than eight times the Sun’s mass runs out of fuel, its core collapses, rebounds, and explodes as a supernova. What’s left behind depends on the star’s mass before the explosion. If it was near the threshold, it creates a city-sized, superdense neutron star. If it had around 20 times the Sun’s mass or more, the star’s core collapses into a stellar-mass black hole.
The masses of these newly born objects can range from a few to hundreds of times the Sun’s mass, depending on star’s mass when the supernova began. Stellar-mass black holes can continue to gain mass through collisions with stars and other black.
Nearly all the stellar-mass black holes observed so far have been found because they’re paired with stars. They likely originated as mismatched stars where the more massive one evolved rapidly into a black hole. In some cases, called X-ray binaries, the black hole pulls gas off the star into a disk that heats up enough to produce X-rays. Binaries have revealed around 50 suspected or confirmed stellar-mass black holes in the Milky Way, but scientists think there may be as many as 100 million in our galaxy alone.
Almost every large galaxy, including our Milky Way, has a supermassive black hole at its center. These monster objects have hundreds of thousands to billions of times the Sun’s mass, although some scientists place the lower boundary at tens of thousands.
The one at the center of our galaxy, Sagittarius A* (pronounced ey-star), is 4 million times the mass of the Sun – relatively small compared to those found in some other galaxies. For example, the black hole at the center of galaxy Holmberg 15A holds at least 40 billion solar masses.
Scientists aren’t sure how these monster objects came to be.
Observations of distant galaxies show that some supermassive black holes formed in the first billion years after the birth of the universe. It’s possible these black holes began with the collapse of supermassive stars in the early universe, which gave them a head start.
While their origins are mysterious, scientists know supermassive black holes can grow by feeding on smaller objects, like their stellar-mass relatives and neutron stars. They can also merge with other supermassive black holes when galaxies collide.
Scientists are puzzled by the size gap between stellar-mass and supermassive black holes.
They think there should be a continuum of sizes because, over cosmic time, collisions between stellar-mass black holes should have created some intermediate-mass black holes. These should range from around one hundred to hundreds of thousands of times the Sun’s mass – or tens of thousands, depending on how supermassive black holes are defined. Scientists are actively hunting for examples of these so-called missing-link black holes. Numerous candidates have been identified but have proven difficult to confirm.
Scientists theorize that primordial black holes formed in the first second after the birth of the universe. In that moment, pockets of hot material may have been dense enough to form black holes, potentially with masses ranging from 100,000 times less than a paperclip to 100,000 times more than the Sun’s. Then as the universe quickly expanded and cooled, the conditions for forming black holes this way ended.
Now, 13.8 billion years later, scientists haven’t yet found definitive proof these primordial black holes ever existed. It’s possible, however, that they could have evaporated as the cosmos aged due to quantum mechanical processes occurring at the edges of their event horizons. According to theoretical predictions, lower-mass black holes (those with less mass than a mountain) would evaporate more quickly than larger ones, which could mean many of these early black holes have completely dissipated. But more massive primordial black holes could still linger across the universe.
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Blind holes are holes that get drilled or milled to a specified depth but do not go all the way through the part.
Thru holes get drilled all the way through a part.
They can be specified as “thru” as shown in the example or the blueprint can make it clear visually that the hole goes all the way through the part.
This picture of a part cut in half shows the difference between a thru hole and a blind hole. The three holes on the left are blind holes which do not break through to the other surface.
The thru hole on the right goes all the way through the part.
The diameter of the hole is the size. The diameter is the distance across the hole.
Less often, holes are specified with a radial dimension instead of a diameter. The radius is the distance from the center of the hole to the edge of the hole. This is equal to 1/2 of the diameter.
The depth of the hole is the distance that it is drilled to.
Holes often get counterbores that allow a fastener such as a bolt head to be recessed.
Holes with a counterbore will specify the size and depth of the hole as well as the size and depth of the counterbore.
Countersinks get added to holes as either a way to specify a chamfer for protective purposes or to allow a fastener such as a screw head to be recessed.
Holes with a countersink will specify the size and depth of the hole as well as the size and angle of the countersink.
Spotfaces are functionally no different than a counterbore. They are machined on a part to allow a fastener to sit flush, though not always completely recessed.
Holes with a spotface will specify the size and depth of the holes as well as the size and depth of the spotface.
Note: spotfaces are not always specified with the symbol shown. At times, they will only use the counterbore symbol and other times they will use the SF notation only.
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Parts and Features > Features > Holes > Advanced Holes > Advanced Hole Type PropertyManager
You cannot drag elements between stacks.
If the drag operation causes a failed element, that
element is highlighted. Hover over the element to display an error
message.
Other options related to using baseline
dimensions include:
For a counterbore, countersink, or taper
threaded element, you can select Use standard
depth to ensure that the depth of the
element is the same depth defined in the Hole Wizard
data table.
For a straight threaded element, you can
select a formula from a list to calculate its
depth.
With the Advanced Hole tool, you can define advanced holes
from the near and far side faces. Hole element flyouts help guide the process.
Specify these options on the Type
tab.
You can customize hole callouts that match the order and variables required for manufacturing, then use the callouts in manufacturing drawings.
To reorder the callouts, select the Callout String and click Move Up and Move Down .
To restore the default options for individual Callout String items, right-click a string and click Restore Default String .
Manage a list of styles for advanced holes that you can reuse in models.
The options available and their icons vary depending on the advanced hole type
selected in the element flyout and the values defined within this Element
Specification section.
End Condition . Select one of the following:
Available from Near Side only, Far Side only, or from both sides. Available for the last element in the Near Side flyout if Far Side is selected. Extends this element to the nearest face of the first element in the Far Side flyout.
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Insert Element Above Active Element
Insert Element Below Active Element
Flips the direction of the near side stack. Available for the Near Side stack only.
Near Side and Far Side Counterbore
Removes all customizations you made to all hole callouts in the PropertyManager.
Resets to No Favorite Selected and the
default options.
Adds the selected advanced hole to the Favorites list. Saves the file as Style (*.sldahstl) . To add a style, click , type
a name, then click OK .
To update a style, edit the properties on the Type ,
select the hole in Favorites , then
click
and enter a new or existing name.
Saves the selected style. Click this option, then browse to a folder. You can edit the file name.
Loads the style. Click this option, browse to a folder, then select a style.
Select one or more faces or planes to sketch on
Displays a temporary preview of the hole on the selected plane or face. The preview does not determine the hole position. Use the Positions tab to position the holes.
Select a face or plane. Available when you select one
or no items. Activates the Far Side values in
the element flyout. Use the flyout to add or delete elements. Define
element values under Element
Specification .
The last element from the Near Side (blue) is set to Blind . The first element from the Far Side (green) is set to Up To Next Element . The depth of the green element is defined from the end of the yellow element till it meets the blue element, in the direction shown by the arrow. The depth of the green element adjusts to remain in contact with the yellow and blue elements.
The last element from the Near Side (blue) and the first element from the Far Side (green) are both set to Up To Next Element . The depth of each element is the total distance between the red and yellow elements divided by two. The depth of both elements adjusts to remain in contact with the yellow and red elements.
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