Broadband traveling wave tubes in Ka- and Ku-band

Ehret, P.; Laurent, Alain; Bosch, E.

doi:10.1109/ivec.2014.6857483

Cited by 3 publications

(4 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Taking the Cassini experiment as a reference, in which a Kα-band travelling wave tube amplifier (TWTA) on board the spacecraft had an output power of 10 W for a distance of 5 AU [25], therefore for the distance of 1.5 AU as in DOCS, an amplifier roughly needs an output power of 10 × (1.5/5) 2 W ≈ 1 W. This amplifier can be easily satisfied, e.g. today the most advanced amplifier in space for Kα-band communication can reach an output of 250 W with a bandwidth of 2.9 GHz [48,49]. However, in Cassini project a 4 meter diameter antenna on board the spacecraft, and especially a 34 meter diameter antenna receiver on ground were used to keep a decent low thermal noise level [25].…”

Section: Technical Issues To Be Solvedmentioning

confidence: 99%

“…This amplifier can be easily satisfied, e.g. today the most advanced amplifier in space for Kα-band communication can reach an output of 250 W with a bandwidth of 2.9 GHz[48,49]. However, in Cassini project a 4 meter diameter antenna on board the spacecraft, and especially a 34 meter diameter antenna receiver on ground were used to keep a decent low thermal noise level[25].It is not yet clear for DOCS if we could achieve a similar or even lower noise level by using similar antennas on board of the two spacecrafts (i.e.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Low-frequency gravitational wave detection via double optical clocks in space

Wang

Wang³

et al. 2018

Class. Quantum Grav.

View full text Add to dashboard Cite

We propose a Doppler tracking system for gravitational wave detection via Double Optical Clocks in Space (DOCS). In this configuration two spacecrafts (each containing an optical clock) are launched to space for Doppler shift observations. Compared to the similar attempt of gravitational wave detection in the Cassini mission, the radio signal of DOCS that contains the relative frequency changes avoids completely noise effects due for instance to troposphere, ionosphere, ground-based antenna and transponder. Given the high stabilities of the two optical clocks (Allan deviation ∼ 4.1 × 10 −17 @ 1000 s), an overall estimated sensitivity of 5 × 10 −19 could be achieved with an observation time of 2 years, and would allow to detect gravitational waves in the frequency range from ∼ 10 −4 Hz to ∼ 10 −2 Hz.

show abstract

Section: Technical Issues To Be Solvedmentioning

confidence: 99%

mentioning

confidence: 99%

Low-frequency gravitational wave detection via double optical clocks in space

Wang

Wang³

et al. 2018

Class. Quantum Grav.

View full text Add to dashboard Cite

show abstract

“…FLIGHT Current developments of very high power TWTs are on going in Europe with broadband designs covering the complete Ku-Band (10.7 to 12.7 GHz) with output powers of up to 300 W. These broadband developments can be in addition optimized for narrowband applications [14]. In the Ka-band the new designs will cover almost 3 GHz of bandwidth (from 17.25 GHz to 20.25 GHz) with power levels in the range of 250 W [14].…”

Section: IVmentioning

confidence: 99%

“…In the Ka-band the new designs will cover almost 3 GHz of bandwidth (from 17.25 GHz to 20.25 GHz) with power levels in the range of 250 W [14].…”

Section: IVmentioning

confidence: 99%

Microwave high power amplifier technologies for space-borne applications

Ayllon

2015

2015 IEEE 16th Annual Wireless and Microwave Technology Conference (WAMICON)

View full text Add to dashboard Cite

This work discusses the main challenges when designing Solid-State Power Amplifiers and Travelling-Wave Tube Amplifiers for space-borne applications. Some examples of flight-proven High Power Amplifiers are given together with on going developments and future trends towards high throughput satellites services (e.g. 3D-TV), that demand the use of higher frequency bands and increased levels of RF output power at the same time.

show abstract