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Advanced Composition Explorer

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Advanced Composition Explorer
An artist's concept of ACE.
Mission typeSolar research
OperatorNASA
COSPAR ID1997-045A Edit this at Wikidata
SATCAT no.24912
Websitewww.srl.caltech.edu/ACE/
Mission duration5 years planned
Elapsed: 27 years, 2 months and 15 days
Spacecraft properties
BusCustom
ManufacturerJohns Hopkins Applied Physics Laboratory
Launch mass757 kilograms (1,669 lb)
Dry mass562 kilograms (1,239 lb)
Power444 W End-of-Life (5 years)
Start of mission
Launch dateAugust 25, 1997, 14:39:00 (1997-08-25UTC14:39Z) UTC
RocketDelta II 7920-8
Launch siteCape Canaveral, LC-17A
Orbital parameters
Reference systemHeliocentric
RegimeL1 Lissajous
Semi-major axis148,100,000 kilometers (92,000,000 mi)
Eccentricity~0.017
Perigee altitude145,700,000 kilometres (90,500,000 mi)
Apogee altitude150,550,000 kilometres (93,550,000 mi)
Inclination~0°
Period1 year
ACE in orbit around the Sun–Earth L1 point.

Advanced Composition Explorer (ACE) is a NASA Explorers program Solar and space exploration mission to study matter comprising energetic particles from the solar wind, the interplanetary medium, and other sources.

Real-time data from ACE is used by the NOAA Space Weather Prediction Center to improve forecasts and warnings of solar storms.[1] The ACE robotic spacecraft was launched August 25, 1997, and entered a Lissajous orbit close to the L1 Lagrangian point (which lies between the Sun and the Earth at a distance of some 1.5 million km from the latter) on December 12, 1997.[2] The spacecraft is currently operating at that orbit. Because ACE is in a non-Keplerian orbit, and has regular station-keeping maneuvers, the orbital parameters in the adjacent information box are only approximate.

As of 2019, the spacecraft is still in generally good condition, and is projected to have enough propellant to maintain its orbit until 2024.[3] NASA Goddard Space Flight Center managed the development and integration of the ACE spacecraft.[4]

Science objectives

ACE observations allow the investigation of a wide range of fundamental problems in the following four major areas:[5]

Elemental and isotopic composition of matter

A major objective is the accurate and comprehensive determination of the elemental and isotopic composition of the various samples of "source material" from which nuclei are accelerated. These observations have been used to:

  • Generate a set of solar isotopic abundances based on a direct sampling of solar material
  • Determine the coronal elemental and isotopic composition with greatly improved accuracy
  • Establish the pattern of isotopic differences between galactic cosmic ray and solar system matter
  • Measure the elemental and isotopic abundances of interstellar and interplanetary "pick–up ions"
  • Determine the isotopic composition of the "anomalous cosmic ray component", which represents a sample of the local interstellar medium

Origin of the elements and subsequent evolutionary processing

Isotopic "anomalies" in meteorites indicate that the solar system was not homogeneous when formed. Similarly, the Galaxy is neither uniform in space nor constant in time due to continuous stellar nucleosynthesis. ACE measurements have been used to:

  • Search for differences between the isotopic composition of solar and meteoritic material
  • Determine the contributions of solar–wind and solar energetic particles to lunar and meteoritic material, and to planetary atmospheres and magnetospheres
  • Determine the dominant nucleosynthetic processes that contribute to cosmic ray source material
  • Determine whether cosmic rays are a sample of freshly synthesized material (e.g., from supernovae) or of the contemporary interstellar medium
  • Search for isotopic patterns in solar and Galactic material as a test of galactic evolution models

Formation of the solar corona and acceleration of the solar wind

Solar energetic particle, solar wind, and spectroscopic observations show that the elemental composition of the corona is differentiated from that of the photosphere, although the processes by which this occurs, and by which the solar wind is subsequently accelerated, are poorly understood. The detailed composition and charge–state data provided by ACE are used to:

  • Isolate the dominant coronal formation processes by comparing a broad range of coronal and photospheric abundances
  • Study plasma conditions at the source of solar wind and solar energetic particles by measuring and comparing the charge states of these two populations
  • Study solar wind acceleration processes and any charge or mass-dependent fractionation in various types of solar wind flows

Particle acceleration and transport in nature

Particle acceleration is ubiquitous in nature and understanding its nature is one of the fundamental problems of space plasma astrophysics. The unique data set obtained by ACE measurements have been used to:

  • Make direct measurements of charge and/or mass-dependent fractionation during solar energetic particle and interplanetary acceleration events
  • Constrain solar flare, coronal shock, and interplanetary shock acceleration models with charge, mass, and spectral data spanning up to five decades in energy
  • Test theoretical models for 3He–rich flares and solar γ–ray events

Instrumentation

Cosmic-Ray Isotope Spectrometer (CRIS)

The Cosmic-Ray Isotope Spectrometer covers the highest decade of the Advanced Composition Explorer's energy interval, from 50 to 500 MeV/nucleon, with an isotopic resolution for elements from Z ≈ 2 to 30. The nuclei detected in this energy interval are predominantly cosmic rays originating in our Galaxy. This sample of galactic matter investigates the nucleosynthesis of the parent material, as well as fractionation, acceleration, and transport processes that these particles undergo in the Galaxy and in the interplanetary medium. Charge and mass identification with CRIS is based on multiple measurements of dE/dx and total energy in stacks of silicon detectors, and trajectory measurements in a scintillating optical fiber trajectory (SOFT) hodoscope. The instrument has a geometrical factor of 250 cm2 sr for isotope measurements.[6]

Solar Isotope Spectrometer (SIS)

The Solar Isotope Spectrometer (SIS) provides high-resolution measurements of the isotopic composition of energetic nuclei from He to Zn (Z = 2 to 30) over the energy range from ~10 to ~100 MeV/nucleon. During large solar events, SIS measures the isotopic abundances of solar energetic particles to determine directly the composition of the solar corona and to study particle acceleration processes. During solar quiet times, SIS measures the isotopes of low-energy cosmic rays from the Galaxy and isotopes of the anomalous cosmic ray component, which originates in the nearby interstellar medium. SIS has two telescopes composed of silicon solid-state detectors that provide measurements of the nuclear charge, mass, and kinetic energy of incident nuclei. Within each telescope, particle trajectories are measured with a pair of two-dimensional silicon strip detectors instrumented with custom very-large-scale integrated (VLSI) electronics to provide both position and energy-loss measurements. SIS was specially designed to achieve excellent mass resolution under the extreme, high flux conditions encountered in large solar particle events. It provides a geometry factor of 40 cm2 sr, significantly greater than earlier solar particle isotope spectrometers.[7]

Ultra-Low-Energy Isotope Spectrometer (ULEIS)

The Ultra-Low-Energy Isotope Spectrometer (ULEIS) on the ACE spacecraft is an ultra-high-resolution mass spectrometer that measures particle composition and energy spectra of elements He–Ni with energies from ~45 keV/nucleon to a few MeV/nucleon. ULEIS investigates particles accelerated in solar energetic particle events, interplanetary shocks, and at the solar wind termination shock. By determining energy spectra, mass composition, and temporal variations in conjunction with other ACE instruments, ULEIS greatly improves our knowledge of solar abundances, as well as other reservoirs such as the local interstellar medium. ULEIS combines the high sensitivity required to measure low particle fluxes, along with the capability to operate in the largest solar particle or interplanetary shock events. In addition to detailed information for individual ions, ULEIS features a wide range of count rates for different ions and energies that allows accurate determination of particle fluxes and anisotropies over short (few minutes) time scales.[8]

Solar Energetic Particle Ionic Charge Analyzer (SEPICA)

The Solar Energetic Particle Ionic Charge Analyzer (SEPICA) was the instrument on the Advanced Composition Explorer (ACE) that determined the ionic charge states of solar and interplanetary energetic particles in the energy range from ≈0.2 MeV nucl-1 to ≈5 MeV charge-1. The charge state of energetic ions contains key information to unravel source temperatures, acceleration, fractionation, and transport processes for these particle populations. SEPICA had the ability to resolve individual charge states with a substantially larger geometric factor than its predecessor ULEZEQ on ISEE-1 and -3, on which SEPICA was based. To achieve these two requirements at the same time, SEPICA was composed of one high-charge resolution sensor section and two low- charge resolution, but large geometric factor sections.[9]

As of 2008, this instrument is no longer functioning due to failed gas valves.[3]

Solar Wind Ion Mass Spectrometer (SWIMS) and Solar Wind Ion Composition Spectrometer (SWICS)

The Solar Wind Ion Composition Spectrometer (SWICS) and the Solar Wind Ions Mass Spectrometer (SWIMS) on ACE are instruments optimized for measurements of the chemical and isotopic composition of solar and interstellar matter. SWICS determined uniquely the chemical and ionic-charge composition of the solar wind, the thermal and mean speeds of all major solar wind ions from H through Fe at all solar wind speeds above 300 km s−1 (protons) and 170 km s−1 (Fe+16), and resolved H and He isotopes of both solar and interstellar sources. SWICS also measured the distribution functions of both the interstellar cloud and dust cloud pickup ions up to energies of 100 keV e−1. SWIMS measures the chemical, isotopic and charge state composition of the solar wind for every element between He and Ni. Each of the two instruments are time-of-flight mass spectrometers and use electrostatic analysis followed by the time-of-flight and, as required, an energy measurement.[10][11]

On August 23, 2011, the SWICS time-of-flight electronics experienced an age- and radiation-induced hardware anomaly that increased the level of background in the composition data. To mitigate the effects of this background, the model for identifying ions in the data was adjusted to take advantage of only the ion energy-per-charge as measured by the electrostatic analyzer, and the ion energy as measured by solid-state detectors. This has allowed SWICS to continue to deliver a subset of the data products that were provided to the public prior to the hardware anomaly, including ion charge state ratios of oxygen and carbon, and measurements of solar wind iron. The measurements of proton density, speed, and thermal speed by SWICS were not affected by this anomaly and continue to the present day.[3]

Electron, Proton, and Alpha-particle Monitor (EPAM)

The Electron, Proton, and Alpha Monitor (EPAM) instrument on the ACE spacecraft is designed to measure a broad range of energetic particles over nearly the full unit-sphere at high time resolution. Such measurements of ions and electrons in the range of a few tens of keV to several MeV are essential to understand the dynamics of solar flares, co-rotating interaction regions (CIR's), interplanetary shock acceleration, and upstream terrestrial events. The large dynamic range of EPAM extends from about 50 keV to 5 MeV for ions, and 40 keV to about 350 keV for electrons. To complement its electron and ion measurements, EPAM is also equipped with a Composition Aperture (CA) which unambiguously identifies ion species reported as species group rates and/or individual pulse-height events. The instrument achieves its large spatial coverage through five telescopes oriented at various angles to the spacecraft spin axis. The low-energy particle measurements, obtained as time resolutions between 1.5 and 24 s, and the ability of the instrument to observe particle anisotropies in three dimensions make EPAM an excellent resource to provide the interplanetary context for studies using other instruments on the ACE spacecraft. [12]

Solar Wind Electron, Proton and Alpha Monitor (SWEPAM)

The Solar Wind Electron Proton Alpha Monitor (SWEPAM) experiment provides the bulk solar wind observations for the Advanced Composition Explorer (ACE). These observations provide the context for elemental and isotopic composition measurements made on ACE as well as allowing the direct examination of numerous solar wind phenomena such as coronal mass ejection, interplanetary shocks, and solar wind fine structure, with advanced, 3-D plasma instrumentation. They also provide an ideal data set for both heliospheric and magnetospheric multi-spacecraft studies where they can be used in conjunction with other, simultaneous observations from spacecraft such as Ulysses. The SWEPAM observations are made simultaneously with independent electron (SWEPAM-e) and ion (SWEPAM-i) instruments. In order to save costs for the ACE project, SWEPAM-e and SWEPAM-i are the recycled flight spares from the joint NASA/ESA Ulysses mission. Both instruments had selective refurbishment, modification, and modernization required to meet the ACE mission and spacecraft requirements. Both incorporate electrostatic analyzers whose fan-shaped fields of view sweep out all pertinent look directions as the spacecraft spins.[13]

Magnetometer (MAG)

The magnetic field experiment on ACE provides continuous measurements of the local magnetic field in the interplanetary medium. These measurements are essential in the interpretation of simultaneous ACE observations of energetic and thermal particle distributions. The experiment consists of a pair of twin, boom- mounted, triaxial flux gate sensors which are located 165 inches (419 cm) from the center of the spacecraft on opposing solar panels. The two triaxial sensors provide a balanced, fully redundant vector instrument and permit some enhanced assessment of the spacecraft's magnetic field. [14]

ACE Real-Time Solar Wind (RTSW)

The Advanced Composition Explorer (ACE) RTSW system is continuously monitoring the solar wind and producing warnings of impending major geomagnetic activity, up to one hour in advance. Warnings and alerts issued by NOAA allow those with systems sensitive to such activity to take preventative action. The RTSW system gathers solar wind and energetic particle data at high time resolution from four ACE instruments (MAG, SWEPAM, EPAM, and SIS), packs the data into a low-rate bit stream, and broadcasts the data continuously. NASA sends real-time data to NOAA each day when downloading science data. With a combination of dedicated ground stations (CRL in Japan and RAL in Great Britain), and time on existing ground tracking networks (NASA's DSN and the USAF's AFSCN), the RTSW system can receive data 24 hours per day throughout the year. The raw data are immediately sent from the ground station to the Space Weather Prediction Center in Boulder, Colorado, processed, and then delivered to its Space Weather Operations Center where they are used in daily operations; the data are also delivered to the CRL Regional Warning Center at Hiraiso, Japan, to the USAF 55th Space Weather Squadron, and placed on the World Wide Web. The data are downloaded, processed and dispersed within 5 min from the time they leave ACE. The RTSW system also uses the low-energy energetic particles to warn of approaching interplanetary shocks, and to help monitor the flux of high-energy particles that can produce radiation damage in satellite systems.[15]

Science results

The spectra of particles observed by ACE

An oxygen fluences observed by ACE.

The figure shows the particle fluence (total flux over a given period of time) of oxygen at ACE for a time period just after solar minimum, the part of the 11-year solar cycle when solar activity is lowest.[16] The lowest-energy particles come from the slow and fast solar wind, with speeds from about 300 to about 800 km/s. Like the solar wind distribution of all ions, that of oxygen has a suprathermal tail of higher-energy particles; that is, in the frame of the bulk solar wind, the plasma has an energy distribution that is approximately a thermal distribution but has a notable excess above about 5 keV, as shown in Figure 1. The ACE team has made contributions to understanding the origins of these tails and their role in injecting particles into additional acceleration processes.

At energies higher than those of the solar wind particles, ACE observes particles from regions known as corotating interaction regions (CIRs). CIRs form because the solar wind is not uniform. Due to solar rotation, high-speed streams collide with preceding slow solar wind, creating shock waves at roughly 2–5 astronomical units (AU, the distance between Earth and the Sun) and forming CIRs. Particles accelerated by these shocks are commonly observed at 1 AU below energies of about 10 MeV per nucleon. ACE measurements confirm that CIRs include a significant fraction of singly charged helium formed when interstellar neutral helium is ionized.[17]

At yet higher energies, the major contribution to the measured flux of particles is due to solar energetic particles (SEPs) associated with interplanetary (IP) shocks driven by fast coronal mass ejections (CMEs) and solar flares. Enriched abundances of helium-3 and helium ions show that the suprathermal tails are the main seed population for these SEPs.[18] IP shocks traveling at speeds up to about 2000 km/s accelerate particles from the suprathermal tail to 100 MeV per nucleon and more. IP shocks are particularly important because they can continue to accelerate particles as they pass over ACE and thus allow shock acceleration processes to be studied in situ.

Other high-energy particles observed by ACE are anomalous cosmic rays (ACRs) that originate with neutral interstellar atoms that are ionized in the inner heliosphere to make "pickup" ions and are later accelerated to energies greater than 10 MeV per nucleon in the outer heliosphere. ACE also observes pickup ions directly; they are easily identified because they are singly charged. Finally, the highest-energy particles observed by ACE are the galactic cosmic rays (GCRs), thought to be accelerated by shock waves from supernova explosions in our galaxy.

Other findings from ACE

Shortly after launch, the SEP sensors on ACE detected solar events that had unexpected characteristics. Unlike most large, shock-accelerated SEP events, these were highly enriched in iron and helium-3, as are the much smaller, flare-associated impulsive SEP events.[19][20] Within the first year of operations, ACE found many of these "hybrid" events, which led to substantial discussion within the community as to what conditions could generate them.[21]

One remarkable recent discovery in heliospheric physics has been the ubiquitous presence of suprathermal particles with common spectral shape. This shape unexpectedly occurs in the quiet solar wind; in disturbed conditions downstream from shocks, including CIRs; and elsewhere in the heliosphere. These observations have led Fisk and Gloeckler [22] to suggest a novel mechanism for the particles' acceleration.

Another discovery has been that the current solar cycle, as measured by sunspots, CMEs, and SEPs, has been much less magnetically active than the previous cycle. McComas et al.[23] have shown that the dynamic pressures of the solar wind measured by the Ulysses satellite over all latitudes and by ACE in the ecliptic plane are correlated and were declining in time for about 2 decades. They concluded that the Sun had been undergoing a global change that affected the overall heliosphere. Simultaneously, GCR intensities were increasing and in 2009 were the highest recorded during the past 50 years.[24] GCRs have more difficulty reaching Earth when the Sun is more magnetically active, so the high GCR intensity in 2009 is consistent with a globally reduced dynamic pressure of the solar wind.

ACE also measures abundances of cosmic ray nickel-59 and cobalt-59 isotopes; these measurements indicate that a time longer than the half-life of nickel-59 with bound electrons (7.6 × 104 years) elapsed between the time nickel-59 was created in a supernova explosion and the time cosmic rays were accelerated.[25] Such long delays indicate that cosmic rays come from the acceleration of old stellar or interstellar material rather than from fresh supernova ejecta. ACE also measures an iron-58/iron-56 ratio that is enriched over the same ratio in solar system material.[26] These and other findings have led to a theory of the origin of cosmic rays in galactic superbubbles, formed in regions where many supernovae explode within a few million years. Recent observations of a cocoon of freshly accelerated cosmic rays in the Cygnus superbubble by the Fermi gamma-ray observatory[27] support this theory.

Follow-on space weather observatory

On February 11, 2015, the Deep Space Climate Observatory (DSCOVR)—with several similar instruments including a newer and more sensitive instrument to detect Earth-bound coronal mass ejections—successfully launched by NOAA and NASA aboard a SpaceX Falcon 9 launch vehicle from Cape Canaveral, Florida. The spacecraft arrived at L1 by June 8, 2015, just over 100 days after launch.[28] Along with ACE, both will provide space weather data as long as ACE can continue to function.[29]

See also

References

  1. ^ "Satellite to aid space weather forecasting". USA Today. June 24, 1999. Archived from the original on October 18, 2009. Retrieved October 24, 2008.
  2. ^ http://www.srl.caltech.edu/ACE/ASC/DATA/ace_dly_reprts/HTML/December_text_1997.html#97346
  3. ^ a b c Christian, Eric R.; Davis, Andrew J. (February 10, 2017). "Advanced Composition Explorer (ACE) Mission Overview". California Institute of Technology. Retrieved December 14, 2017.
  4. ^ NASA - NSSDC - Spacecraft - Details
  5. ^ Stone, E.C.; et al. (July 1998). "The Advanced Composition Explorer". Space Science Reviews. 86: 1–22. Bibcode:1998SSRv...86....1S. doi:10.1023/A:1005082526237.
  6. ^ Stone, E.C.; et al. (July 1998). "The Cosmic-Ray Isotope Spectrometer for the Advanced Composition Explorer". Space Science Reviews. 86: 285–356. Bibcode:1998SSRv...86..285S. CiteSeerX 10.1.1.38.7241. doi:10.1023/A:1005075813033.
  7. ^ Stone, E.C.; et al. (July 1998). "The Solar Isotope Spectrometer for the Advanced Composition Explorer". Space Science Reviews. 86: 357–408. Bibcode:1998SSRv...86..357S. doi:10.1023/A:1005027929871.
  8. ^ Mason, G.M.; et al. (July 1998). "The Ultra-Low-Energy Isotope Spectrometer (ULEIS) for the Advanced Composition Explorer". Space Science Reviews. 86: 409–448. Bibcode:1998SSRv...86..409M. doi:10.1023/A:1005079930780.
  9. ^ Moebius, E.; et al. (July 1998). "The Solar Energetic Particle Ionic Charge Analyzer (SEPICA) and the Data Processing Unit (S3DPU) for SWICS, SWIMS and SEPICA". Space Science Reviews. 86: 449–495. Bibcode:1998SSRv...86..449M. doi:10.1023/A:1005084014850.
  10. ^ Gloeckler, G.; et al. (July 1998). "Investigation of the composition of solar and interstellar matter using solar wind and pickup ion measurements with SWICS and SWIMS on the ACE spacecraft". Space Science Reviews. 86: 497–539. Bibcode:1998SSRv...86..497G. doi:10.1023/A:1005036131689.
  11. ^ "ACE/SWICS & ACE/SWIMS". The Solar and Heliospheric Research Group. Archived from the original on August 10, 2006. Retrieved June 30, 2006.
  12. ^ Gold, R.E.; et al. (July 1998). "Electron, Proton, and Alpha Monitor on the Advanced Composition Explorer Spacecraft". Space Science Reviews. 86: 541–562. Bibcode:1998SSRv...86..541G. doi:10.1023/A:1005088115759.
  13. ^ McComas, D.J.; et al. (July 1998). "Solar Wind Electron Proton Alpha Monitor (SWEPAM) for the Advanced Composition Explorer". Space Science Reviews. 86: 563–612. Bibcode:1998SSRv...86..563M. doi:10.1023/A:1005040232597.
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  16. ^ Mewaldt, R.A.; et al. (2001). "Long-term fluences of energetic particles in the heliosphere" (PDF). AIP Conf. Proc. 86: 165–170. Bibcode:2001AIPC..598..165M. doi:10.1063/1.1433995. hdl:2027.42/87586.
  17. ^ Möbius, E.; et al. (2002). "Charge states of energetic (~ 0.5 MeV/n) ions in corotating interaction regions at 1 AU and implications on source populations". Geophys. Res. Lett. 29 (2): 1016. Bibcode:2002GeoRL..29.1016M. doi:10.1029/2001GL013410.
  18. ^ Desai, M.I.; et al. (2001). "Acceleration of 3He nuclei at interplanetary shocks". Astrophysical Journal. 553 (1): L89–L92. Bibcode:2001ApJ...553L..89D. doi:10.1086/320503.
  19. ^ Cohen, C.M.S.; et al. (1999). "Inferred charge states of high energy solar particles from the solar isotope spectrometer on ACE" (PDF). Geophys. Res. Lett. 26 (2): 149–152. Bibcode:1999GeoRL..26..149C. doi:10.1029/1998GL900218.
  20. ^ Mason, G.M.; et al. (1999). "Particle acceleration and sources in the November 1997 solar energetic particle events" (PDF). Geophys. Res. Lett. 26 (2): 141–144. Bibcode:1999GeoRL..26..141M. doi:10.1029/1998GL900235.
  21. ^ Cohen, C.M.S.; et al. (2012). "Observations of the longitudinal spread of solar energetic particle events in solar cycle 24" (PDF). AIP Conf. Proc. 1436: 103–109. Bibcode:2012AIPC.1436..103C. doi:10.1063/1.4723596.
  22. ^ Fisk, L.A.; et al. (2008). "Acceleration of suprathermal tails in the solar wind". Astrophysical Journal. 686 (2): 1466–1473. Bibcode:2008ApJ...686.1466F. doi:10.1086/591543.
  23. ^ McComas, D.J.; et al. (2008). "Weaker solar wind from the polar coronal holes and the whole Sun". Geophys. Res. Lett. 35 (18): L18103. Bibcode:2008GeoRL..3518103M. doi:10.1029/2008GL034896. S2CID 14927209.
  24. ^ Leske, R.A.; et al. (2011). "Anomalous and galactic cosmic rays at 1 AU during the cycle 23/24 solar minimum". Space Sci. Rev. 176 (1–4): 253–263. Bibcode:2013SSRv..176..253L. doi:10.1007/s11214-011-9772-1.
  25. ^ Wiedenbeck, M.E.; et al. (1999). "Constraints on the time delay between nucleosynthesis and cosmic-ray acceleration from observations of 59Ni and 59Co". Astrophysical Journal. 523 (1): L61–L64. Bibcode:1999ApJ...523L..61W. doi:10.1086/312242.
  26. ^ Binns, W.R.; et al. (2005). "Cosmic-ray neon, Wolf-Rayet stars, and the superbubble origin of galactic cosmic rays". Astrophysical Journal. 634 (1): 351–364. arXiv:astro-ph/0508398. Bibcode:2005ApJ...634..351B. doi:10.1086/496959.
  27. ^ Ackermann, M.; et al. (2011). "A cocoon of freshly accelerated cosmic rays detected by Fermi in the Cygnus superbubble". Science. 334 (6059): 1103–7. Bibcode:2011Sci...334.1103A. doi:10.1126/science.1210311. PMID 22116880. S2CID 38789717.
  28. ^ "Nation's first operational satellite in deep space reaches final orbit". NOAA. June 8, 2015. Archived from the original on June 8, 2015. Retrieved June 8, 2015.
  29. ^ Graham, William (February 8, 2015). "SpaceX Falcon 9 ready for DSCOVR mission". NASASpaceFlight.com. Retrieved February 8, 2015.
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