Radar astronomy

• Control of attributes of the signal [i.e., the waveform's time/frequency modulation and polarization]
• Resolve objects spatially.
• Delay-Doppler measurement precision.
• Optically opaque penetration.
• Sensitive to high concentrations of metal or ice.

The maximum range of astronomy by radar is very limited, and is confined to the Solar System. This is because the signal strength drops off very steeply with distance to the target, the small fraction of incident flux that is reflected by the target, and the limited strength of transmitters.{{Cite book | last = Hey | first = J. S. | title = The Evolution of Radio Astronomy | publisher = Paul Elek (Scientific Books) | series = Histories of Science Series | volume = 1 | date = 1973 }} The distance to which the radar can detect an object is proportional to the square root of the object's size, due to the one-over-distance-to-the-fourth dependence of echo strength. Radar could detect something ~1 km across a large fraction of an AU away, but at 8-10 AU, the distance to Saturn, we need targets at least hundreds of kilometers wide. It is also necessary to have a relatively good ephemeris of the target before observing it.

The Moon is comparatively close and was detected by radar soon after the invention of the technique in 1946.{{cite journal |first=Jack |last=Mofensen |url=http://www.eagle.ca/~harry/ba/eme/index.htm |title=Radar echoes from the moon |archive-url=https://web.archive.org/web/20081029000712/http://www.eagle.ca/~harry/ba/eme/index.htm |archive-date=2008-10-29 |journal=Electronics |volume=19 |pages=92–98 |date=April 1946}}{{cite journal |first=Zoltán |last=Bay |author-link=Zoltán Lajos Bay |title=Reflection of microwaves from the moon |journal=Hungarica Acta Physica |volume=1 |issue=1 |pages=1–22 |date=January 1947 |doi=10.1007/BF03161123 |doi-access=free |url=https://link.springer.com/content/pdf/10.1007/BF03161123.pdf}} Measurements included surface roughness and later mapping of shadowed regions near the poles.

The next easiest target is Venus. This was a target of great scientific value, since it could provide an unambiguous way to measure the size of the astronomical unit, which was needed for the nascent field of interplanetary spacecraft. In addition such technical prowess had great public relations value, and was an excellent demonstration to funding agencies. So there was considerable pressure to squeeze a scientific result from weak and noisy data, which was accomplished by heavy post-processing of the results, utilizing the expected value to tell where to look. This led to early claims (from Lincoln Laboratory,{{cite journal

|title=Radar Echoes from Venus: Advances in several arts made possible this experiment in radio astronomy performed during the IGY

|last1=Price |first1=R |last2=Green Jr |first2=PE |last3=Goblick Jr |first3=TJ |last4=Kingston |first4=RH

|last5=Kraft Jr |first5=LG |last6=Pettengill |first6=GH |last7=Silver |first7=R |last8=Smith |first8=WB

|journal=Science

|volume=129

|issue=3351

|pages=751--753

|year=1959

|publisher=American Association for the Advancement of Science

|url=https://www.science.org/doi/pdf/10.1126/science.129.3351.751}} Jodrell Bank,{{cite journal

|title=Radio echo observations of Venus

|last1=Evans |first1=JV |last2=Taylor |first2=GN

|journal=Nature

|volume=184

|issue=4696

|pages=1358--1359

|year=1959

|publisher=Nature Publishing Group UK London}} and Vladimir A. Kotelnikov of the USSR{{cite journal

|title=Radar contact with Venus

|last1=Kotelnokov |first1=VA

|journal=Journal of the British Institution of Radio Engineers

|volume=22

|issue=4

|pages=293--295

|year=1961

|publisher=IET

|url=http://vak.rutgers.edu/Chapters_T2/020_060%20Radar%20Contact%20with%20Venus%20(1961).pdf}}) which are now known to be incorrect. All of these agreed with each other and the conventional value of AU at the time, {{val|149467000|u=km}}.{{cite book |url=https://history.nasa.gov/SP-4218/sp4218.htm |title=NASA SP-4218: To See the Unseen - A History of Planetary Radar Astronomy |chapter=Chapter 2: Fickle Venus |chapter-url=http://history.nasa.gov:80/SP-4218/ch2.htm |first=Andrew J. |last=Butrica |publisher = NASA | date=1996 |access-date=2008-05-15 |archive-url=https://web.archive.org/web/20070823124845/https://history.nasa.gov/SP-4218/sp4218.htm |archive-date=2007-08-23 |url-status=live}}

The first unambiguous detection of Venus was made by the Jet Propulsion Laboratory on 10 March 1961. JPL established contact with the planet Venus using a planetary radar system from 10 March to 10 May 1961. Using both velocity and range data, a new value of {{val|149598500|500|u=km}} was determined for the astronomical unit.

{{cite journal

| last1 = Malling | first1 = L. R. |last2 = Golomb |first2 = S. W.

| title = Radar Measurements of the Planet Venus

| journal = Journal of the British Institution of Radio Engineers| volume = 22 | issue = 4 | pages = 297–300

| date = October 1961

| url = https://ieeexplore.ieee.org/document/5259664

| archive-url = https://web.archive.org/web/20180125020130/http://ieeexplore.ieee.org/document/5259664/

| url-status = dead

| archive-date = January 25, 2018

| doi = 10.1049/jbire.1961.0121

| format = PDF

| url-access = subscription

}}{{cite journal

| title=The astronomical unit determined by radar reflections from Venus

| last1=Muhleman |first1=Duane O. |last2=Holdridge |first2=D. B. |last3=Block |first3=N.

| journal=Astronomical Journal |volume=67 |issue=4 |pages=191–203 |date=May 1962

| doi=10.1086/108693 |bibcode=1962AJ.....67..191M

|doi-access=free }} Using further analysis, this gives a refined figure of {{val|149598845|250|u=km}}. Once the correct value was known, other groups found echos in their archived data that agreed with these results.

The Sun has been detected several times starting in 1959. Frequencies are usually between 25 and 38 MHz, much lower than for interplanetary work. Reflections from both the photosphere and the corona were detected.{{Cite web |last=Ohlson |first=John E. |date=August 1967 |title=A RADAR INVESTIGATION OF THE SOLAR CORONA |url=https://ntrs.nasa.gov/api/citations/19680007049/downloads/19680007049.pdf |website=NASA Technical Reports Server}}

The following is a list of planetary bodies that have been observed by this means:

• Mercury - Improved value for the distance from the earth observed (GR test). Rotational period, libration, surface mapping, esp. of polar regions.
• Venus - first radar detection in 1961. Rotation period, gross surface properties. The Magellan mission mapped the entire planet using a radar altimeter.
• Earth - numerous airborne and spacecraft radars have mapped the entire planet, for various purposes. One example is the Shuttle Radar Topography Mission, which mapped large parts of the surface of Earth at 30 m resolution.
• Mars - Mapping of surface roughness from Arecibo Observatory. The Mars Express mission carries a ground-penetrating radar.
• Jupiter System - Galilean satellites
• Saturn System - Rings and Titan from Arecibo Observatory, mapping of Titan's surface and observations of other moons from the Cassini spacecraft.

Image:Asteroid-Kleopatra-radar.png, based on radar analysis.]]

Image:Radar images and computer model of asteroid 1999 JM8.jpg

Radar provides the ability to study the shape, size and spin state of asteroids and comets from the ground. Radar imaging has produced images with up to 7.5-meter resolution. With sufficient data, the size, shape, spin and radar albedo of the target asteroids can be extracted.

As of 2016, only 19 comets had been studied by radar, including 73P/Schwassmann-Wachmann, along with radar observations of 612 Near-Earth asteroids and 138 Main belt asteroids.{{cite web|url = http://echo.jpl.nasa.gov/asteroids/|title = Radar-Detected Asteroids and Comets|publisher = NASA/JPL Asteroid Radar Research|access-date = 2016-04-25}} By 2025, this had grown to 138 main-belt asteroids, 1148 near-Earth asteroids, and 23 comets.

Many bodies are observed during their close flyby of Earth.

While operational the Arecibo Observatory provided information about Earth threatening comet and asteroid impacts, allowing impact and near miss predictions decades into the future such as those for Apophis and other bodies. Being smaller, the Goldstone Solar System Radar is less sensitive and unable to provide the same predictive capacity.

The Goldstone Solar System Radar is the only planetary radar in current regular operation.{{cite journal

|title=Planetary radar—State-of-the-art review

|last1= Virkki |first1= Anne K. |last2= Neish |first2= Catherine D. |last3= Rivera-Valentín |first3= Edgard G.

|last4= Bhiravarasu |first4= Sriram S. |last5= Hickson |first5= Dylan C. |last6= Nolan |first6= Michael C.

|last7= Orosei |first7= Roberto

|journal=Remote Sensing

|volume=15

|issue=23

|pages=5605

|year=2023

|publisher=MDPI

|url=https://www.mdpi.com/2072-4292/15/23/5605 }} Others are or were:

• The planetary radar at Arecibo Observatory, which collapsed in 2020.
• The Soviet planetary radar at the Pluton complex, since dismantled.
• The Millstone Hill and Haystack radio telescopes of the Haystack Observatory made radar observations from 1958 through at least 1970.{{cite journal

|title=The Haystack Planetary Ranging Radar

|last1=Evans |first1=JV |last2=Ingalls |first2=RP |last3=Pettengill |first3=GH

|journal=Technical Report-Jet Propulsion Laboratory, California Institute of Technology

|issue=32

|pages=27

|year=1970

|publisher=Jet Propulsion Laboratory, California Institute of Technology}}

• The Yevpatoria RT-70 radio telescope is equipped with a powerful transmitter, and has been used in bi-static radar observations.{{cite web |url=https://www.ursi.org/proceedings/procGA02/papers/p1745.pdf |title=BISTATIC RADAR TEST ACTIVITIES AT THE ITALIAN MEDICINA RADIOTELESCOPES}}

There are proposals and prototypes for possible additional radars:

• The Green Bank Observatory is investigating a Ku-band radar for its 100 meter radio telescope.{{cite web |url=https://amostech.com/TechnicalPapers/2022/Poster/Taylor.pdf |title=The next generation planetary radar system on the Green Bank Telescope}} Its low power prototype has imaged the moon.
• China is developing a planetary radar.{{cite web |url=https://www.tsinghua.edu.cn/en/info/1320/11412.htm |title=China begins construction on world’s most far-reaching radar system, to boost defense against near-Earth asteroid impact}} Their initial phase has imaged the moon.

{{Commons category}}

• Radar
• 6489 Golevka
• 4179 Toutatis

{{Reflist}}

• [http://www.planetary.org/blog/article/00003248/ How radio telescopes get images of asteroids] {{Webarchive|url=https://web.archive.org/web/20120125070636/http://www.planetary.org/blog/article/00003248/ |date=2012-01-25 }}
• {{cite web |url=http://www.naic.edu/%7Epradar/pradar.htm |title=Planetary Radar at Arecibo Observatory |publisher=NAIC |access-date=2008-05-15 |archive-date=2008-05-14 |archive-url=https://web.archive.org/web/20080514034816/http://www.naic.edu/%7Epradar/pradar.htm |url-status=dead }}
• {{cite web |url=http://deepspace.jpl.nasa.gov/technology/95_20/gold.htm |title=Goldstone Solar System Radar |publisher=JPL |access-date=2010-09-28 |url-status=dead |archive-url=https://web.archive.org/web/20101021074837/http://deepspace.jpl.nasa.gov/technology/95_20/gold.htm |archive-date=2010-10-21 }}
• {{cite web |url=http://echo.jpl.nasa.gov/ |title=JPL Asteroid Radar Research |author=Dr. Steven J. Ostro |author2=Dr. Lance A. M. Benner |name-list-style=amp |publisher=Caltech |date=2007 |access-date=2008-05-15}}
• {{cite web |url=http://www.cplire.ru/html/ra&sr/index.html |title=Radar Astronomy and Space Radio Science |access-date=2008-05-15}}
• {{cite web |url=http://www2.ess.ucla.edu/~jlm/research/NEAs/intro.html |title=Introduction to Asteroid Radar Astronomy | author=Dr. Jean-Luc Margot |publisher=UCLA |access-date=2013-08-02}}
• [https://web.archive.org/web/20040608071121/http://echo.jpl.nasa.gov/~lance/binary.neas.html BINARY AND TERNARY NEAR-EARTH ASTEROIDS DETECTED BY RADAR]

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Category:Observational astronomy

Category:Radar