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| last_contact =
| last_contact =
| deactivated = 12 January 2012
| deactivated = 12 January 2012
| decay_date = 30 April 2018 <ref>{{cite web|title=NASA's Rossi X-ray Timing Explorer Leaves Scientific "Treasure Trove"|date=May 2018 |url=https://www.nasa.gov/feature/goddard/2018/nasas-rossi-x-ray-timing-explorer-leaves-scientific-treasure-trove|publisher=NASA|access-date=3 May 2018}} {{PD-notice}}</ref>
| decay_date = 30 April 2018 <ref>{{cite web |title=NASA's Rossi X-ray Timing Explorer Leaves Scientific "Treasure Trove" |date=May 2018 |url=https://www.nasa.gov/feature/goddard/2018/nasas-rossi-x-ray-timing-explorer-leaves-scientific-treasure-trove |publisher=NASA |access-date=3 May 2018}} {{PD-notice}}</ref>


| orbit_reference = [[Geocentric orbit]]<ref name="Trajectory">{{cite web|url=https://nssdc.gsfc.nasa.gov/nmc/spacecraft/displayTrajectory.action?id=1995-074A|title=Trajectory: X-Ray Timing Explorer (1995-074A) Explorer 69|publisher=NASA|date=28 October 2021|access-date=28 November 2021}} {{PD-notice}}</ref>
| orbit_reference = [[Geocentric orbit]]<ref name="Trajectory">{{cite web |url=https://nssdc.gsfc.nasa.gov/nmc/spacecraft/displayTrajectory.action?id=1995-074A |title=Trajectory: X-Ray Timing Explorer (1995-074A) Explorer 69 |publisher=NASA |date=28 October 2021 |access-date=28 November 2021}} {{PD-notice}}</ref>
| orbit_regime = [[Low Earth orbit]]
| orbit_regime = [[Low Earth orbit]]
| orbit_periapsis = {{cvt|409|km}}
| orbit_periapsis = {{cvt|409|km}}
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}}
}}


The '''Rossi X-ray Timing Explorer''' ('''RXTE''') was a [[NASA]] satellite that observed the time variation of astronomical X-ray sources, named after physicist [[Bruno Rossi]]. The RXTE had three instruments — an All Sky Monitor, the High-Energy X-ray Timing Experiment (HEXTE) and the Proportional Counter Array. The RXTE observed X-rays from [[black holes]], [[neutron stars]], [[X-ray pulsars]] and [[X-ray bursts]]. It was funded as part of the [[Explorer program]], and was also called '''Explorer 69'''.
The '''Rossi X-ray Timing Explorer''' ('''RXTE''') was a [[NASA]] satellite that observed the time variation of astronomical X-ray sources, named after physicist [[Bruno Rossi]]. The RXTE had three instruments — an All-Sky Monitor, the High-Energy X-ray Timing Experiment (HEXTE) and the Proportional Counter Array. The RXTE observed X-rays from [[black holes]], [[neutron stars]], [[X-ray pulsars]] and [[X-ray bursts]]. It was funded as part of the [[Explorer program]] and was also called '''Explorer 69'''.


RXTE had a mass of {{cvt|3200|kg}} and was launched from [[Cape Canaveral Space Force Station|Cape Canaveral]] on 30 December 1995, at 13:48:00 [[Coordinated Universal Time|UTC]], on a [[Delta (rocket family)|Delta II]] [[launch vehicle]]. Its [[International Designator]] is 1995-074A.<ref name="Display">{{cite web|url=https://nssdc.gsfc.nasa.gov/nmc/spacecraft/display.action?id=1995-074A|title=Display: X-Ray Timing Explorer (1995-074A) Explorer 69|publisher=NASA|date=28 October 2021|access-date=28 November 2021}} {{PD-notice}}</ref>
RXTE had a mass of {{cvt|3200|kg}} and was launched from [[Cape Canaveral Space Force Station|Cape Canaveral]] on 30 December 1995, at 13:48:00 [[Coordinated Universal Time|UTC]], on a [[Delta II]] [[launch vehicle]]. Its [[International Designator]] is 1995-074A.<ref name="Display">{{cite web |url=https://nssdc.gsfc.nasa.gov/nmc/spacecraft/display.action?id=1995-074A |title=Display: X-Ray Timing Explorer (1995-074A) Explorer 69 |publisher=NASA |date=28 October 2021 |access-date=28 November 2021}} {{PD-notice}}</ref>


== Mission ==
== Mission ==
The X-Ray Timing Explorer (XTE) mission has the primary objective to study the temporal and broad-band spectral phenomena associated with stellar and galactic systems containing compact objects in the energy range 2--200 KeV, and in time scales from microseconds to years. The scientific instruments consists of two pointed instruments, the Proportional Counter Array (PCA) and the High-Energy X-ray Timing Experiment (HEXTE), and the All Sky Monitor (ASM), which scans over 70% of the sky each orbit. All of the XTE observing time were available to the international scientific community through a peer review of submitted proposals. XTE used a new spacecraft design that allows flexible operations through rapid pointing, high data rates, and nearly continuous receipt of data at the Science Operations Center (SOC) at Goddard Space Flight Center via a Multiple Access link to the [[Tracking and Data Relay Satellite System]] (TDRSS). XTE was highly maneuverable with a slew rate of greater than 6° per minute. The PCA/HEXTE could be pointed anywhere in the sky to an accuracy of less than 0.1°, with an aspect knowledge of around 1 [[Minute and second of arc|arcminute]]. Rotatable solar panels enable anti-sunward pointing to coordinate with ground-based night-time observations. Two pointable high gain antennas maintain nearly continuous communication with the TDRSS. This, together with 1 [[Gigabit|GB]] (approximately four orbits) of on-board solid-state data storage, give added flexibility in scheduling observations.<ref name="Display"/>
The X-Ray Timing Explorer (XTE) mission has the primary objective to study the temporal and broad-band spectral phenomena associated with stellar and galactic systems containing compact objects in the energy range 2--200 KeV and in time scales from microseconds to years. The scientific instruments consists of two pointed instruments, the Proportional Counter Array (PCA) and the High-Energy X-ray Timing Experiment (HEXTE), and the All Sky Monitor (ASM), which scans over 70% of the sky each orbit. All of the XTE observing time were available to the international scientific community through a peer review of submitted proposals. XTE used a new spacecraft design that allows flexible operations through rapid pointing, high data rates, and nearly continuous receipt of data at the Science Operations Center (SOC) at Goddard Space Flight Center via a Multiple Access link to the [[Tracking and Data Relay Satellite System]] (TDRSS). XTE was highly maneuverable with a slew rate of greater than 6° per minute. The PCA/HEXTE could be pointed anywhere in the sky to an accuracy of less than 0.1°, with an aspect knowledge of around 1 [[Minute and second of arc|arcminute]]. Rotatable solar panels enable anti-sunward pointing to coordinate with ground-based night-time observations. Two pointable high-gain antennas maintain nearly continuous communication with the TDRSS. This, together with 1 [[Gigabit|GB]] (approximately four orbits) of on-board solid-state data storage, give added flexibility in scheduling observations.<ref name="Display"/>


== Telecommunications ==
== Telecommunications ==
* Required continuous TDRSS Multiple Access (MA) return link coverage except for zone of exclusion: Real time and playback of engineering/housekeeping data at 16 or 32 kbs - Playback of science data at 48 or 64 kbs.<ref name="Telecommunications">{{cite web|url=https://nssdc.gsfc.nasa.gov/nmc/spacecraft/displayTelemetry.action?id=1995-074A|title=Telecommunications Description|publisher=NASA|date=28 October 2021|access-date=28 November 2021}} {{PD-notice}}</ref>
* Required continuous TDRSS Multiple Access (MA) return link coverage except for zone of exclusion: Real-time and playback of engineering/housekeeping data at 16 or 32 kbs - Playback of science data at 48 or 64 kbs.<ref name="Telecommunications">{{cite web |url=https://nssdc.gsfc.nasa.gov/nmc/spacecraft/displayTelemetry.action?id=1995-074A |title=Telecommunications Description |publisher=NASA |date=28 October 2021 |access-date=28 November 2021}} {{PD-notice}}</ref>
* Requires 20 minutes of SSA contacts with alternating TDRSS per orbit: Real time and playback of engineering/housekeeping data at 32 kbs - Playback of science data at 512 or 1024 kbs.
* Requires 20 minutes of SSA contacts with alternating TDRSS per orbit: Real-time and playback of engineering/housekeeping data at 32 kbs - Playback of science data at 512 or 1024 kbs.
* For launch and contingency, required TDRSS MA/SSA real time engineering and housekeeping at 1 kbs.
* For launch and contingency, required TDRSS MA/SSA real-time engineering and housekeeping at 1 kbs.
* The bit error rate shall be less than 1 in 10E8 for at least 95% of the orbits.
* The bit error rate shall be less than 1 in 10E8 for at least 95% of the orbits.


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=== All-Sky Monitor (ASM) ===
=== All-Sky Monitor (ASM) ===
The All-Sky Monitor (ASM) provided all-sky X-ray coverage, to a sensitivity of a few percent of the [[Crab Nebula]] intensity in one day, in order to provide both flare alarms and long-term intensity records of celestial X-ray sources.<ref name="Experiment1">{{cite web|url=https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1995-074A-01|title=Experiment: All-Sky Monitor (ASM)|publisher=NASA|date=28 October 2021|access-date=28 November 2021}} {{PD-notice}}</ref> The ASM consisted of three wide-angle shadow cameras equipped with proportional counters with a total collecting area of {{cvt|90|cm2}}. The instrumental properties were:<ref>{{cite web|url=http://heasarc.gsfc.nasa.gov/docs/xte/ASM.html|title=All-Sky Monitor (ASM)|publisher=Heasarc.gsfc.nasa.gov|date=2002-02-04|access-date=2012-02-03}} {{PD-notice}}</ref><ref name="ASM">{{cite web|url=https://heasarc.gsfc.nasa.gov/docs/xte/asm_products_guide.html|title=The RXTE All Sky Monitor Data Products|publisher=NASA|date=26 August 1997|access-date=28 November 2021}} {{PD-notice}}</ref>
The All-Sky Monitor (ASM) provided all-sky X-ray coverage, to a sensitivity of a few percent of the [[Crab Nebula]] intensity in one day, in order to provide both flare alarms and long-term intensity records of celestial X-ray sources.<ref name="Experiment1">{{cite web |url=https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1995-074A-01 |title=Experiment: All-Sky Monitor (ASM) |publisher=NASA |date=28 October 2021 |access-date=28 November 2021}} {{PD-notice}}</ref> The ASM consisted of three wide-angle shadow cameras equipped with proportional counters with a total collecting area of {{cvt|90|cm2}}. The instrumental properties were:<ref>{{cite web |url=http://heasarc.gsfc.nasa.gov/docs/xte/ASM.html |title=All-Sky Monitor (ASM) |publisher=Heasarc.gsfc.nasa.gov |date=2002-02-04 |access-date=2012-02-03}} {{PD-notice}}</ref><ref name="ASM">{{cite web |url=https://heasarc.gsfc.nasa.gov/docs/xte/asm_products_guide.html |title=The RXTE All Sky Monitor Data Products |publisher=NASA |date=26 August 1997 |access-date=28 November 2021}} {{PD-notice}}</ref>


* Energy range: 2–12-keV
* Energy range: 2–12-keV;
* Time resolution: observes 80% of the sky every 90 minutes
* Time resolution: observes 80% of the sky every 90 minutes;
* Spatial resolution: 3' × 15'
* Spatial resolution: 3' × 15';
* Number of shadow cameras: 3, each with 6° × 90° FoV
* Number of shadow cameras: 3, each with 6° × 90° FoV;
* Collecting area: {{cvt|90|cm2}}
* Collecting area: {{cvt|90|cm2}};
* Detector: [[Xenon]] proportional counter, position-sensitive
* Detector: [[Xenon]] proportional counter, position-sensitive;
* Sensitivity: 30 [[Crab (unit)|mCrab]]
* Sensitivity: 30 [[Crab (unit)|mCrab]].


It was built by the CSR at [[Massachusetts Institute of Technology]]. The [[principal investigator]] was [http://web.mit.edu/physics/people/faculty/bradt_hale.html Dr. Hale Bradt].
It was built by the CSR at [[Massachusetts Institute of Technology]]. The [[principal investigator]] was [http://web.mit.edu/physics/people/faculty/bradt_hale.html Dr. Hale Bradt].


=== High Energy X-ray Timing Experiment (HEXTE) ===
=== High Energy X-ray Timing Experiment (HEXTE) ===
The High-Energy X-ray Timing Experiment (HEXTE) is a scintillator array for the study of temporal and temporal/spectral effects of the hard X-ray (20 to 200 keV) emission from galactic and extragalactic sources.<ref name="Experiment3">{{cite web|url=https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1995-074A-03|title=Experiment: High Energy X-ray Timing Experiment (HEXTE)|publisher=NASA|date=28 October 2021|access-date=28 November 2021}} {{PD-notice}}</ref> The HEXTE consisted of two clusters each containing four [[phoswich detector|phoswich scintillation detectors]]. Each cluster could "rock" (beamswitch) along mutually orthogonal directions to provide background measurements 1.5° or 3.0° away from the source every 16 to 128 seconds. In addition, the input was sampled at 8 [[microsecond]]s so as to detect time varying phenomena. Automatic gain control was provided by using an {{SimpleNuclide|americium|241|link=yes}} radioactive source mounted in each detector's field of view. The HEXTE's basic properties were:<ref>{{cite web |url=http://heasarc.gsfc.nasa.gov/docs/xte/HEXTE.html|title=High Energy X-ray Timing Experiment (HEXTE)|publisher=NASA|date=1999-09-14|access-date=2012-02-03}} {{PD-notice}}</ref>
The High-Energy X-ray Timing Experiment (HEXTE) is a scintillator array for the study of temporal and temporal/spectral effects of the hard X-ray (20 to 200 keV) emission from galactic and extragalactic sources.<ref name="Experiment3">{{cite web |url=https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1995-074A-03 |title=Experiment: High Energy X-ray Timing Experiment (HEXTE) |publisher=NASA |date=28 October 2021 |access-date=28 November 2021}} {{PD-notice}}</ref> The HEXTE consisted of two clusters each containing four [[phoswich detector|phoswich scintillation detectors]]. Each cluster could "rock" (beam switch) along mutually orthogonal directions to provide background measurements 1.5° or 3.0° away from the source every 16 to 128 seconds. In addition, the input was sampled at 8 [[microsecond]]s so as to detect time-varying phenomena. Automatic gain control was provided by using an {{SimpleNuclide|americium|241|link=yes}} radioactive source mounted in each detector's field of view. The HEXTE's basic properties were:<ref>{{cite web |url=http://heasarc.gsfc.nasa.gov/docs/xte/HEXTE.html |title=High Energy X-ray Timing Experiment (HEXTE) |publisher=NASA |date=1999-09-14 |access-date=2012-02-03}} {{PD-notice}}</ref>


* Energy range: 15–250-keV
* Energy range: 15–250 keV;
* Energy resolution: 15% at 60-keV
* Energy resolution: 15% at 60 keV;
* Time sampling: 8 microseconds
* Time sampling: 8 microseconds;
* Field of view: 1° FWHM
* Field of view: 1° [[Full width at half maximum|FWHM]];
* Detectors: 2 clusters of 4 NaI/CsI [[scintillation counter]]s
* Detectors: 2 clusters of 4 NaI/CsI [[scintillation counter]]s;
* Collecting area: 2 × {{cvt|800|cm2}}
* Collecting area: 2 × {{cvt|800|cm2}};
* Sensitivity: 1-Crab = 360 count/second per HEXTE cluster
* Sensitivity: 1-Crab = 360 count/second per HEXTE cluster;
* Background: 50 count/second per HEXTE cluster
* Background: 50 count/second per HEXTE cluster.


The HEXTE was designed and built by the [http://cass.ucsd.edu Center for Astrophysics & Space Sciences (CASS)] at the [[University of California, San Diego]]. The HEXTE principal investigator was [https://web.archive.org/web/20081229041202/http://mamacass.ucsd.edu/people/rrothschild.html Dr. Richard E. Rothschild].
The HEXTE was designed and built by the [http://cass.ucsd.edu Center for Astrophysics & Space Sciences (CASS)] at the [[University of California, San Diego]]. The HEXTE principal investigator was [https://web.archive.org/web/20081229041202/http://mamacass.ucsd.edu/people/rrothschild.html Dr. Richard E. Rothschild].


=== Proportional Counter Array (PCA) ===
=== Proportional Counter Array (PCA) ===
The Proportional Counter Array (PCA) provides approximately {{cvt|6500|cm2}} of X-ray detector area, in the energy range 2 to 60 keV, for the study of temporal/spectral effects in the X-ray emission from galactic and extragalactic sources.<ref name="Experiment2">{{cite web|url=https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1995-074A-02|title=Experiment: Proportional Counter Array (PCA) |publisher=NASA|date=28 October 2021|access-date=28 November 2021}} {{PD-notice}}</ref> The PCA was an array of five proportional counters with a total collecting area of {{cvt|6500|cm2}}. The instrumental properties were:<ref name="HEASARC">{{cite web|url=https://heasarc.gsfc.nasa.gov/docs/xte/learning_center/pca.html|title=Proportional Counter Array (PCA)|publisher=NASA|date=2011-12-06|access-date=2018-10-05}}</ref>
The Proportional Counter Array (PCA) provides approximately {{cvt|6500|cm2}} of X-ray detector area, in the energy range 2 to 60 keV, for the study of temporal/spectral effects in the X-ray emission from galactic and extragalactic sources.<ref name="Experiment2">{{cite web |url=https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1995-074A-02 |title=Experiment: Proportional Counter Array (PCA) |publisher=NASA |date=28 October 2021 |access-date=28 November 2021}} {{PD-notice}}</ref> The PCA was an array of five proportional counters with a total collecting area of {{cvt|6500|cm2}}. The instrumental properties were:<ref name="HEASARC">{{cite web |url=https://heasarc.gsfc.nasa.gov/docs/xte/learning_center/pca.html |title=Proportional Counter Array (PCA) |publisher=NASA |date=2011-12-06 |access-date=2018-10-05}}</ref>


* Energy range: 2–60-keV
* Energy range: 2–60 keV;
* Energy resolution: <18% at 6-keV
* Energy resolution: <18% at 6 keV;
* Time resolution: 1-μs
* Time resolution: 1 μs
* Spatial resolution: collimator with 1° [[Full width at half maximum]] (FWHM)
* Spatial resolution: collimator with 1° (FWHM);
* Detectors: 5 proportional counters
* Detectors: 5 proportional counters;
* Collecting area: {{cvt|6500|cm2}}
* Collecting area: {{cvt|6500|cm2}};
* Layers: 1 [[propane]] veto; 3 [[Xenon]], each split into two; 1 Xenon veto layer
* Layers: 1 [[propane]] veto; 3 [[Xenon]], each split into two; 1 Xenon veto layer;
* Sensitivity: 0.1-mCrab
* Sensitivity: 0.1-mCrab;
* Background: 90-mCrab
* Background: 90-mCrab.


The PCA is being built by the Laboratory for High Energy Astrophysics (LHEA) at [[Goddard Space Flight Center]]. The principal investigator was [[Jean Swank|Jean H. Swank]].<ref name="HEASARC"/>
The PCA is being built by the Laboratory for High Energy Astrophysics (LHEA) at [[Goddard Space Flight Center]]. The principal investigator was [[Jean Swank]].<ref name="HEASARC"/>


== Results ==
== Results ==
Observations from the Rossi X-ray Timing Explorer have been used as evidence for the existence of the [[frame-dragging]] effect predicted by the theory of [[general relativity]] of [[Albert Einstein|Einstein]]. RXTE results have, as of late 2007, been used in more than 1400 scientific papers.
Observations from the Rossi X-ray Timing Explorer have been used as evidence for the existence of the [[frame-dragging]] effect predicted by the theory of [[general relativity]] of [[Albert Einstein|Einstein]]. RXTE results have, as of late 2007, been used in more than 1400 scientific papers.


In January 2006, it was announced that Rossi had been used to locate a candidate [[intermediate-mass black hole]] named [[M82 X-1]].<ref>{{cite news |url=http://www.scienceblog.com/cms/dying_star_reveals_more_evidence_for_new_kind_of_black_hole_9685|title=Dying Star Reveals More Evidence for New Kind of Black Hole|newspaper=Scienceblog.com |date=8 January 2006 |publisher=Science Blog|access-date=2012-02-03|last1=Com |first1=Scienceblog }}</ref> In February 2006, data from RXTE was used to prove that the diffuse background X-ray glow in our [[galaxy]] comes from innumerable, previously undetected [[white dwarf]]s and from other stars' [[Stellar corona|coronae]].<ref>{{cite web|url=http://skyandtelescope.com/news/article_1681_1.asp|title=Galactic Glow Gleaned}}</ref> In April 2008, RXTE data was used to infer the size of the smallest known black hole.<ref>{{cite web|title=NASA Scientists Identify Smallest Known Black Hole|url=http://www.nasa.gov/centers/goddard/news/topstory/2008/smallest_blackhole.html|date=2008-04-01}} {{PD-notice}}</ref>
In January 2006, it was announced that Rossi had been used to locate a candidate [[intermediate-mass black hole]] named [[M82 X-1]].<ref>{{cite news |url=http://www.scienceblog.com/cms/dying_star_reveals_more_evidence_for_new_kind_of_black_hole_9685 |title=Dying Star Reveals More Evidence for New Kind of Black Hole |newspaper=Scienceblog.com |date=8 January 2006 |publisher=Science Blog |access-date=2012-02-03 |last1=Com |first1=Scienceblog}}</ref> In February 2006, data from RXTE was used to prove that the diffuse background X-ray glow in our [[galaxy]] comes from innumerable, previously undetected [[white dwarf]]s and from other stars' [[Stellar corona|coronae]].<ref>{{cite web |url=http://skyandtelescope.com/news/article_1681_1.asp |title=Galactic Glow Gleaned}}</ref> In April 2008, RXTE data was used to infer the size of the smallest known black hole.<ref>{{cite web |title=NASA Scientists Identify Smallest Known Black Hole |url=http://www.nasa.gov/centers/goddard/news/topstory/2008/smallest_blackhole.html |date=2008-04-01}} {{PD-notice}}</ref>


RXTE ceased science operations on 12 January 2012.<ref>{{cite web|title=The RXTE Mission is Approaching the End of Science Operations|url=http://heasarc.nasa.gov/docs/xte/xhp_new.html#endofoperations|archive-url=https://web.archive.org/web/20040107162230/http://heasarc.nasa.gov/docs/xte/xhp_new.html#endofoperations|url-status=dead|archive-date=2004-01-07|date=2012-01-04}} {{PD-notice}}</ref>
RXTE ceased science operations on 12 January 2012.<ref>{{cite web |title=The RXTE Mission is Approaching the End of Science Operations |url=http://heasarc.nasa.gov/docs/xte/xhp_new.html#endofoperations |archive-url=https://web.archive.org/web/20040107162230/http://heasarc.nasa.gov/docs/xte/xhp_new.html#endofoperations |url-status=dead |archive-date=2004-01-07 |date=2012-01-04}} {{PD-notice}}</ref>


== Atmospheric entry ==
== Atmospheric entry ==
NASA scientists said that the decommissioned RXTE would re-enter the Earth's atmosphere "between 2014 and 2023".<ref name="Register">{{cite web|url=https://www.theregister.co.uk/2012/01/11/rxte_satellite/ |title=NASA's ageing black hole-stalking probe switched off|website=[[The Register]] |date=11 January 2012|access-date=28 November 2021}}</ref> Later, it became clear that the satellite would re-enter in late April or early May 2018,<ref name="NASA20180425">{{cite web|title=NASA Frequently Asked Questions: RXTE Spacecraft Re-entry|url=https://www.nasa.gov/feature/goddard/2018/nasa-frequently-asked-questions-rxte-spacecraft-re-entry |publisher=NASA|date=25 April 2018|access-date=28 November 2021}}</ref> and the spacecraft fell out of orbit on 30 April 2018.<ref name="SC20180515">{{cite web|url=https://www.space.com/40592-nasa-rxte-satellite-falls-to-earth.html|title=A Pioneering NASA Satellite Just Fell to Earth After 2 Decades in Space|publisher=Space.com|date=15 May 2018|access-date=28 November 2021}}</ref>
NASA scientists said that the decommissioned RXTE would re-enter the Earth's atmosphere "between 2014 and 2023" (30 April 2018).<ref name="Register">{{cite web |url=https://www.theregister.co.uk/2012/01/11/rxte_satellite/ |title=NASA's aging black hole-stalking probe switched off |website=theregister.co.uk |date=11 January 2012 |access-date=28 November 2021}}</ref> Later, it became clear that the satellite would re-enter in late April or early May 2018,<ref name="NASA20180425">{{cite web |title=NASA Frequently Asked Questions: RXTE Spacecraft Re-entry |url=https://www.nasa.gov/feature/goddard/2018/nasa-frequently-asked-questions-rxte-spacecraft-re-entry |publisher=NASA |date=25 April 2018 |access-date=28 November 2021}}</ref> and the spacecraft fell out of orbit on 30 April 2018.<ref name="SC20180515">{{cite web |url=https://www.space.com/40592-nasa-rxte-satellite-falls-to-earth.html |title=A Pioneering NASA Satellite Just Fell to Earth After 2 Decades in Space |publisher=Space.com |date=15 May 2018 |access-date=28 November 2021}}</ref>


== See also ==
== See also ==

Latest revision as of 07:28, 27 July 2024

Rossi X-ray Timing Explorer
RXTE 3D Model
Rossi X-ray Timing Explorer satellite
NamesExplorer 69
RXTE
XTE
Mission typeAstronomy
OperatorNASA
COSPAR ID1995-074A Edit this at Wikidata
SATCAT no.23757
WebsiteRXTE home page
Mission duration16 years (achieved)
Spacecraft properties
SpacecraftExplorer LXVIX
Spacecraft typeRossi X-ray Timing Explorer
BusX-ray Timing Explorer
ManufacturerGoddard Space Flight Center
Launch mass3,200 kg (7,100 lb)
Power800 watts
Start of mission
Launch date30 December 1995, 13:48:00 UTC
RocketDelta II 7920-10 (Delta 230)
Launch siteCape Canaveral, SLC-17A
ContractorMcDonnell Douglas Astronautics Company
Entered service30 December 1995
End of mission
Deactivated12 January 2012
Decay date30 April 2018 [1]
Orbital parameters
Reference systemGeocentric orbit[2]
RegimeLow Earth orbit
Perigee altitude409 km (254 mi)
Apogee altitude409 km (254 mi)
Inclination28.50°
Period92.60 minutes
Instruments
ASM All Sky Monitor (ASM)
HEXTE High-Energy X-ray Timing Experiment (HEXTE)
PCA Proportional Counter Array (PCA)

The Rossi X-ray Timing Explorer (RXTE) was a NASA satellite that observed the time variation of astronomical X-ray sources, named after physicist Bruno Rossi. The RXTE had three instruments — an All-Sky Monitor, the High-Energy X-ray Timing Experiment (HEXTE) and the Proportional Counter Array. The RXTE observed X-rays from black holes, neutron stars, X-ray pulsars and X-ray bursts. It was funded as part of the Explorer program and was also called Explorer 69.

RXTE had a mass of 3,200 kg (7,100 lb) and was launched from Cape Canaveral on 30 December 1995, at 13:48:00 UTC, on a Delta II launch vehicle. Its International Designator is 1995-074A.[3]

Mission

[edit]

The X-Ray Timing Explorer (XTE) mission has the primary objective to study the temporal and broad-band spectral phenomena associated with stellar and galactic systems containing compact objects in the energy range 2--200 KeV and in time scales from microseconds to years. The scientific instruments consists of two pointed instruments, the Proportional Counter Array (PCA) and the High-Energy X-ray Timing Experiment (HEXTE), and the All Sky Monitor (ASM), which scans over 70% of the sky each orbit. All of the XTE observing time were available to the international scientific community through a peer review of submitted proposals. XTE used a new spacecraft design that allows flexible operations through rapid pointing, high data rates, and nearly continuous receipt of data at the Science Operations Center (SOC) at Goddard Space Flight Center via a Multiple Access link to the Tracking and Data Relay Satellite System (TDRSS). XTE was highly maneuverable with a slew rate of greater than 6° per minute. The PCA/HEXTE could be pointed anywhere in the sky to an accuracy of less than 0.1°, with an aspect knowledge of around 1 arcminute. Rotatable solar panels enable anti-sunward pointing to coordinate with ground-based night-time observations. Two pointable high-gain antennas maintain nearly continuous communication with the TDRSS. This, together with 1 GB (approximately four orbits) of on-board solid-state data storage, give added flexibility in scheduling observations.[3]

Telecommunications

[edit]
  • Required continuous TDRSS Multiple Access (MA) return link coverage except for zone of exclusion: Real-time and playback of engineering/housekeeping data at 16 or 32 kbs - Playback of science data at 48 or 64 kbs.[4]
  • Requires 20 minutes of SSA contacts with alternating TDRSS per orbit: Real-time and playback of engineering/housekeeping data at 32 kbs - Playback of science data at 512 or 1024 kbs.
  • For launch and contingency, required TDRSS MA/SSA real-time engineering and housekeeping at 1 kbs.
  • The bit error rate shall be less than 1 in 10E8 for at least 95% of the orbits.

Instruments

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XTE launch
RXTE preparations in 1995

All-Sky Monitor (ASM)

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The All-Sky Monitor (ASM) provided all-sky X-ray coverage, to a sensitivity of a few percent of the Crab Nebula intensity in one day, in order to provide both flare alarms and long-term intensity records of celestial X-ray sources.[5] The ASM consisted of three wide-angle shadow cameras equipped with proportional counters with a total collecting area of 90 cm2 (14 sq in). The instrumental properties were:[6][7]

  • Energy range: 2–12-keV;
  • Time resolution: observes 80% of the sky every 90 minutes;
  • Spatial resolution: 3' × 15';
  • Number of shadow cameras: 3, each with 6° × 90° FoV;
  • Collecting area: 90 cm2 (14 sq in);
  • Detector: Xenon proportional counter, position-sensitive;
  • Sensitivity: 30 mCrab.

It was built by the CSR at Massachusetts Institute of Technology. The principal investigator was Dr. Hale Bradt.

High Energy X-ray Timing Experiment (HEXTE)

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The High-Energy X-ray Timing Experiment (HEXTE) is a scintillator array for the study of temporal and temporal/spectral effects of the hard X-ray (20 to 200 keV) emission from galactic and extragalactic sources.[8] The HEXTE consisted of two clusters each containing four phoswich scintillation detectors. Each cluster could "rock" (beam switch) along mutually orthogonal directions to provide background measurements 1.5° or 3.0° away from the source every 16 to 128 seconds. In addition, the input was sampled at 8 microseconds so as to detect time-varying phenomena. Automatic gain control was provided by using an 241
Am
 radioactive source mounted in each detector's field of view. The HEXTE's basic properties were:[9]

  • Energy range: 15–250 keV;
  • Energy resolution: 15% at 60 keV;
  • Time sampling: 8 microseconds;
  • Field of view: 1° FWHM;
  • Detectors: 2 clusters of 4 NaI/CsI scintillation counters;
  • Collecting area: 2 × 800 cm2 (120 sq in);
  • Sensitivity: 1-Crab = 360 count/second per HEXTE cluster;
  • Background: 50 count/second per HEXTE cluster.

The HEXTE was designed and built by the Center for Astrophysics & Space Sciences (CASS) at the University of California, San Diego. The HEXTE principal investigator was Dr. Richard E. Rothschild.

Proportional Counter Array (PCA)

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The Proportional Counter Array (PCA) provides approximately 6,500 cm2 (1,010 sq in) of X-ray detector area, in the energy range 2 to 60 keV, for the study of temporal/spectral effects in the X-ray emission from galactic and extragalactic sources.[10] The PCA was an array of five proportional counters with a total collecting area of 6,500 cm2 (1,010 sq in). The instrumental properties were:[11]

  • Energy range: 2–60 keV;
  • Energy resolution: <18% at 6 keV;
  • Time resolution: 1 μs
  • Spatial resolution: collimator with 1° (FWHM);
  • Detectors: 5 proportional counters;
  • Collecting area: 6,500 cm2 (1,010 sq in);
  • Layers: 1 propane veto; 3 Xenon, each split into two; 1 Xenon veto layer;
  • Sensitivity: 0.1-mCrab;
  • Background: 90-mCrab.

The PCA is being built by the Laboratory for High Energy Astrophysics (LHEA) at Goddard Space Flight Center. The principal investigator was Jean Swank.[11]

Results

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Observations from the Rossi X-ray Timing Explorer have been used as evidence for the existence of the frame-dragging effect predicted by the theory of general relativity of Einstein. RXTE results have, as of late 2007, been used in more than 1400 scientific papers.

In January 2006, it was announced that Rossi had been used to locate a candidate intermediate-mass black hole named M82 X-1.[12] In February 2006, data from RXTE was used to prove that the diffuse background X-ray glow in our galaxy comes from innumerable, previously undetected white dwarfs and from other stars' coronae.[13] In April 2008, RXTE data was used to infer the size of the smallest known black hole.[14]

RXTE ceased science operations on 12 January 2012.[15]

Atmospheric entry

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NASA scientists said that the decommissioned RXTE would re-enter the Earth's atmosphere "between 2014 and 2023" (30 April 2018).[16] Later, it became clear that the satellite would re-enter in late April or early May 2018,[17] and the spacecraft fell out of orbit on 30 April 2018.[18]

See also

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References

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  1. ^ "NASA's Rossi X-ray Timing Explorer Leaves Scientific "Treasure Trove"". NASA. May 2018. Retrieved 3 May 2018. Public Domain This article incorporates text from this source, which is in the public domain.
  2. ^ "Trajectory: X-Ray Timing Explorer (1995-074A) Explorer 69". NASA. 28 October 2021. Retrieved 28 November 2021. Public Domain This article incorporates text from this source, which is in the public domain.
  3. ^ a b "Display: X-Ray Timing Explorer (1995-074A) Explorer 69". NASA. 28 October 2021. Retrieved 28 November 2021. Public Domain This article incorporates text from this source, which is in the public domain.
  4. ^ "Telecommunications Description". NASA. 28 October 2021. Retrieved 28 November 2021. Public Domain This article incorporates text from this source, which is in the public domain.
  5. ^ "Experiment: All-Sky Monitor (ASM)". NASA. 28 October 2021. Retrieved 28 November 2021. Public Domain This article incorporates text from this source, which is in the public domain.
  6. ^ "All-Sky Monitor (ASM)". Heasarc.gsfc.nasa.gov. 4 February 2002. Retrieved 3 February 2012. Public Domain This article incorporates text from this source, which is in the public domain.
  7. ^ "The RXTE All Sky Monitor Data Products". NASA. 26 August 1997. Retrieved 28 November 2021. Public Domain This article incorporates text from this source, which is in the public domain.
  8. ^ "Experiment: High Energy X-ray Timing Experiment (HEXTE)". NASA. 28 October 2021. Retrieved 28 November 2021. Public Domain This article incorporates text from this source, which is in the public domain.
  9. ^ "High Energy X-ray Timing Experiment (HEXTE)". NASA. 14 September 1999. Retrieved 3 February 2012. Public Domain This article incorporates text from this source, which is in the public domain.
  10. ^ "Experiment: Proportional Counter Array (PCA)". NASA. 28 October 2021. Retrieved 28 November 2021. Public Domain This article incorporates text from this source, which is in the public domain.
  11. ^ a b "Proportional Counter Array (PCA)". NASA. 6 December 2011. Retrieved 5 October 2018.
  12. ^ Com, Scienceblog (8 January 2006). "Dying Star Reveals More Evidence for New Kind of Black Hole". Scienceblog.com. Science Blog. Retrieved 3 February 2012.
  13. ^ "Galactic Glow Gleaned".
  14. ^ "NASA Scientists Identify Smallest Known Black Hole". 1 April 2008. Public Domain This article incorporates text from this source, which is in the public domain.
  15. ^ "The RXTE Mission is Approaching the End of Science Operations". 4 January 2012. Archived from the original on 7 January 2004. Public Domain This article incorporates text from this source, which is in the public domain.
  16. ^ "NASA's aging black hole-stalking probe switched off". theregister.co.uk. 11 January 2012. Retrieved 28 November 2021.
  17. ^ "NASA Frequently Asked Questions: RXTE Spacecraft Re-entry". NASA. 25 April 2018. Retrieved 28 November 2021.
  18. ^ "A Pioneering NASA Satellite Just Fell to Earth After 2 Decades in Space". Space.com. 15 May 2018. Retrieved 28 November 2021.
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